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Collapse of Massive Stars
A MacFadyen
Caltech
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Superbowl Burst
ms variability + non-thermal spectrum Compactness
GRB Light Curve
M = E c2 ~ 10-6
Msun
Gamma-Ray Burstsbull Short -ray flashes E gt 100 keV
bull 001 lt t90 lt 1000s
bull Diverse lightcurvesbull BATSE detected
1day = 1000 yearuniverse
bull Energy ~ 1052 f
-1 ferg
bull Near star forming regions
bull 2 SN Ibc associations
bull Supernova component in lightcurves
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Muller (1999)
ldquoDelayedrdquo SN Explosion
ac
Accretion vs Neutrino heating
Burrows (2001)
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Superbowl Burst
ms variability + non-thermal spectrum Compactness
GRB Light Curve
M = E c2 ~ 10-6
Msun
Gamma-Ray Burstsbull Short -ray flashes E gt 100 keV
bull 001 lt t90 lt 1000s
bull Diverse lightcurvesbull BATSE detected
1day = 1000 yearuniverse
bull Energy ~ 1052 f
-1 ferg
bull Near star forming regions
bull 2 SN Ibc associations
bull Supernova component in lightcurves
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Pre-Supernova Density Structure
Woosley amp Weaver (1995)
Bigger stars
Higher entropy
Shallower density gradients
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Superbowl Burst
ms variability + non-thermal spectrum Compactness
GRB Light Curve
M = E c2 ~ 10-6
Msun
Gamma-Ray Burstsbull Short -ray flashes E gt 100 keV
bull 001 lt t90 lt 1000s
bull Diverse lightcurvesbull BATSE detected
1day = 1000 yearuniverse
bull Energy ~ 1052 f
-1 ferg
bull Near star forming regions
bull 2 SN Ibc associations
bull Supernova component in lightcurves
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Fukuda (1982)
Heger (2000)
Stellar Rotation
no mass lossMass loss
No B fields
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Superbowl Burst
ms variability + non-thermal spectrum Compactness
GRB Light Curve
M = E c2 ~ 10-6
Msun
Gamma-Ray Burstsbull Short -ray flashes E gt 100 keV
bull 001 lt t90 lt 1000s
bull Diverse lightcurvesbull BATSE detected
1day = 1000 yearuniverse
bull Energy ~ 1052 f
-1 ferg
bull Near star forming regions
bull 2 SN Ibc associations
bull Supernova component in lightcurves
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
IFTwo plausible conditions occur
1 Failure of neutrino powered SN explosion
a completeb partial (fallback)
2 Rotating stellar coresj gt 3 x 1016 cm2s
THEN
Rapidly accreting black hole (M~01 Ms)fed by collapsing star (tdyn ~ 446 s frac12 ~ 10 s)Disk formation
COLLAPSAR
Superbowl Burst
ms variability + non-thermal spectrum Compactness
GRB Light Curve
M = E c2 ~ 10-6
Msun
Gamma-Ray Burstsbull Short -ray flashes E gt 100 keV
bull 001 lt t90 lt 1000s
bull Diverse lightcurvesbull BATSE detected
1day = 1000 yearuniverse
bull Energy ~ 1052 f
-1 ferg
bull Near star forming regions
bull 2 SN Ibc associations
bull Supernova component in lightcurves
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Superbowl Burst
ms variability + non-thermal spectrum Compactness
GRB Light Curve
M = E c2 ~ 10-6
Msun
Gamma-Ray Burstsbull Short -ray flashes E gt 100 keV
bull 001 lt t90 lt 1000s
bull Diverse lightcurvesbull BATSE detected
1day = 1000 yearuniverse
bull Energy ~ 1052 f
-1 ferg
bull Near star forming regions
bull 2 SN Ibc associations
bull Supernova component in lightcurves
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Gamma-Ray Burstsbull Short -ray flashes E gt 100 keV
bull 001 lt t90 lt 1000s
bull Diverse lightcurvesbull BATSE detected
1day = 1000 yearuniverse
bull Energy ~ 1052 f
-1 ferg
bull Near star forming regions
bull 2 SN Ibc associations
bull Supernova component in lightcurves
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
135 models (1993)
Note most are Galactic and are ruled out for long bursts
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
GRB 990123
1 CGRO ~1o
2 BeppoSAX (X-ray)
6-33 hrs
34-54 hrs
~ 1rsquo
4 HST 17 days
3 Palomar lt 1 dayKeck
spectrum
z=160
Eiso =
3x1054 erg
~ Msunc2
9th mag flash
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
GRB photons are made far away from engine
Canrsquot observe engine directly in light (neutrinos gravitational waves)
Electromagnetic process or neutrino annihilation to tap power of central compact object
Hyper-accreting black hole or high field neutron star (rotating)
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
SN2003dhGRB030329
Hjorth et al (2003)
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Well-localized bursts are all ldquolong-softrdquo
ldquoshort-hardrdquo bursts
Duration (s)
hardness
Kulkarni et al
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
GRB central engine
bull Relativity (SR amp GR)bull Magnetic Fieldsbull Rotationbull Nuclear Physicsbull Neutrinosbull EOSbull Turbulencebull 3Dbull Range of Lengthscales
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
1st Collapsar Simulations
bull pre-SN 15 Msun Helium starbull Newtonian Hydrodynamics (PPM)bull alpha viscositybull rotationbull photodisintegration (NSE alpha n p)bull neutrino cooling thermal + URCA optically thinbull Ideal nucleons radiation relativistic degenerate
electrons positionsbull 2D axisymmetric spherical gridbull self gravity bull Rin = 9 Rs Rout = 9000 Rs
MacFadyen amp Woosley (1999)
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Heger Langer ampWoosley (1999)
Angular momentum at
Last stable orbit
15 x 1016 cm2 s-1 (Kerr)
46 x 1016 cm2 s-1
(Schwarzschild)
Initial Pre-Supernova Model (KEPLER 25 Msun)
He 806 Msun
Fe 19 Msun
j
T
Collapse velocity = 10000 kms
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Disk Formation Movie
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
= 01 ltMgt = 007 Msun s = 13 x 1053 ergs
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
spin
mass
Use 1D neutrino cooled
ldquoslimrdquo disk models
from Popham et al (1999)
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Ejet = f Maccc2
MHD
T = 57 ms
E = 5 x 1050 ergs
Edep = 28 x 1048 erg
Jet BirthThermal energy deposition focused by toroidal funnel structure
fmax ~ 06 - 4
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Relativistic Jet Movie
Zhang Woosley amp MacFadyen (2003 ApJ March 21)
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Jupiter
Red Supergiant
R~1013 cm
Blue Supergiant
R~1012 cm
Wolf-Rayet Star
R~few x1010 cm
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Relativistic Kelvin-Helmholtz
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
t=7598s
t=7540s
Min
~ 12Mout
=gt OutflowsMacFadyen amp Woosley (1999)
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Nickel Wind Movie
ldquoNickel Windrdquo
T gt 5 x 109 K
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
T = 1010 Kn p
RRkep
(j) = j22GM = 25 x 107 ((jj17
22m33) cm
OO 16
CC12
Si28
He44
++ 1019 erggm
Ni ckel Wi nd
- 1019 erggm
Disk is replenished by collapsing star
tt accrete = t collapse or tt fallback
tt accrete tt drain = mm disk mm
afterburner
Ni56
He44
Disk Outflow Diagram
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Supernovae
Ia
WD cosmology
Type II
Hydrogen
Type I
No Hydrogen
Ib Ic
exploding WR
thermonuclear old pop E galaxies
core collapse massive stars
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Exploding star Supernovae
bull Radioactive decay of Ni56bull tail of Type II ALL of Type Ibull Type I compact star WD or W-R
bull Eexp -gt adiabatic expansion not light
bull no Ni56 -gt no Supernova
bull SN 1998bw amp 2003dh need 05 Msun
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Do all collapsars make supernovaeNo
If Nickel is made in wind it depends on angular momentum of
star1 jisco lt j lt j efficient cooling GRB only
2 j lt j lt j semi-efficient cooling GRB + supernova
3 j gt j inefficient cooling supernova only
j lt jisco nothing
note supernova hypernova (Egt1052 erg M(Ni) gt 03M)
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
NTT image (May 1 1998) of SN 1998bw in the barred spiral galaxy ESO 184-G82 [Galama et al AampAS 138 465 (1999)]
WFC error box (8) for GRB 980425 and two NFI x-ray sources The IPN error arc is also shown
1) Were the two events the same thing
2) Was GRB 980425 an ordinary GRB seen off-axis
SN 1998bwGRB 980425
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
2 ldquoBriefrdquo jet tengine tjet
Engine dies before jet breakout
Mildly relativistic shock breakout
MacFadyen (1999)
What made SN1998bw+GRB980425
1 Accretion powered hypernova w Nickel wind
MacFadyen (2002)
E~ 1052 erg M(Ni)~05 M
GRB from ~3 shock breakout (Tan et al 2001 Perna amp Vietri 2002)
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Fallback in weak SN explosionsShock
reaches surface of star but parts of star are
not ejected to infinity
MacFadyen Woosley amp Heger (2001)
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Fallback accretion Same star exploded with
a range of explosion energies
Significant accretion for thousands of seconds to
days
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Principle Resultsbull Sustained accretion 1 Msuns forgt10sbull Jet formation and collimationbull Sufficient energy for cosmo GRBbull Neutrino cooling amp photodissociation
allows accretionbull Massive bi-conical outflows developbull Time-scale set by He core collapsebull Fallback -gt v long GRB in WR star or
asymmetric SN in SG
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
Conclusions
bull long GRBs from rotating WR stars tengine gt tescape
bull Need SN failure amp angular momentumndash Low metallicity binary can help
bull SN IF nickel is made GRBSN association Type Ibcbull SNGRB ratio may depend on angular momentumbull ldquoNickel windrdquo can explode star -gt hypernova
ndash H env Type II (no GRB) no H Type I + GRBbull Jet instabilities -gt variability intermittancybull Unique nucleosynthesis r-processbull Fallback -gt asymmetric SN very long GRBsbull magnetic models worth attention
