January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 11

Nucleosynthesis, Pulsars, Nucleosynthesis, Pulsars, Cosmic Rays, and Shock Cosmic Rays, and Shock

Physics: High Energy Physics: High Energy Studies of Supernova Studies of Supernova

Remnants with Remnants with ChandraChandra and and XMM-NewtonXMM-Newton

John P. HughesJohn P. Hughes

Rutgers UniversityRutgers University

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 22

Crab Nebula SN1054Crab Nebula SN1054Time spacing ~6 weeks

Polar jet, torus, inner ring (~0.2 pc)

Highly dynamic

Wisps move at ~0.5c

(Hester et al 2002)

PSR spin energy, relativistic wind

Nature of wisps still debated

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 33

New Pulsars and CCOsNew Pulsars and CCOs

Cas ACas A CXOU CXOU J232327.9+584842J232327.9+584842

CCOCCO

PKS 1209-PKS 1209-51/5251/52

1E 1207.4-52091E 1207.4-5209 424 ms (X-424 ms (X-ray)ray)

G106.3+2.7G106.3+2.7 PSR J2229+6114PSR J2229+6114 51.6 ms 51.6 ms (radio)(radio)

IC 443IC 443 CXOU CXOU J061705.3+222127J061705.3+222127

CCOCCO

G292.0+1.8G292.0+1.8 PSR J1124-5916PSR J1124-5916 135 ms 135 ms (radio)(radio)

RX J0852.0-RX J0852.0-46224622

CXOU J085201.4-461753CXOU J085201.4-461753 CCOCCO

3C 583C 58 PSR J0205+6449PSR J0205+6449 65.7 ms (X-65.7 ms (X-ray)ray)

G54.1+0.3G54.1+0.3 PSR J1930+1852PSR J1930+1852 136 ms 136 ms (radio)(radio)

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 44

3C 58 and NS Cooling3C 58 and NS Cooling Crab-like remnantCrab-like remnant Associated with SN 1181Associated with SN 1181 65.68 ms PSR (Murray et 65.68 ms PSR (Murray et

al. 2002)al. 2002) Distance 3.2 kpcDistance 3.2 kpc Spectrum of central Spectrum of central

source (Slane et al. 2002)source (Slane et al. 2002)– Power law: Power law: = 1.7 = 1.7

– TTBBBB < 1.08 x 10 < 1.08 x 1066 K for 12 K for 12 km radius neutron starkm radius neutron star

Below “standard” NS Below “standard” NS cooling curvecooling curve

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 55

Nucleosynthesis in CC SNeNucleosynthesis in CC SNe Hydrostatic nucleosynthesisHydrostatic nucleosynthesis

– During hydrostatic evolution of starDuring hydrostatic evolution of star– Builds up shells rich in H, He, C, O, and SiBuilds up shells rich in H, He, C, O, and Si– Amount of C, O, Ne, Mg ejected varies strongly Amount of C, O, Ne, Mg ejected varies strongly

with progenitor masswith progenitor mass Explosive nucleosynthesisExplosive nucleosynthesis

– Some mechanism drives a shock wave with Some mechanism drives a shock wave with 10105151+ erg through the Fe-core+ erg through the Fe-core

– Burning front T’s of ~10Burning front T’s of ~1099 K cause explosive O- K cause explosive O- and Si-burningand Si-burning

– Only affects the central parts of the star – outer Only affects the central parts of the star – outer layers retain their pre-SN compositionlayers retain their pre-SN composition

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 66

Explosive NucleosynthesisExplosive Nucleosynthesis

ProcessProcess T (10T (1099 K)K) Main ProductsMain Products

Explosive complete Si-Explosive complete Si-burning burning 5.05.0 ““Fe”, HeFe”, He

Explosive incomplete Si-Explosive incomplete Si-burningburning 4.04.0 Si, S, Fe, Ar, CaSi, S, Fe, Ar, Ca

Explosive O-burningExplosive O-burning 3.33.3 O, Si, S, Ar, CaO, Si, S, Ar, Ca

Explosive Ne/C-burningExplosive Ne/C-burning 1.21.2 O, Mg, Si, NeO, Mg, Si, Ne

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 77

Typical Mass FractionsTypical Mass Fractions

ElemenElementt

Ex NeEx Ne Ex OEx O Ex Si-iEx Si-i Ex Si-cEx Si-c

OO 0.720.72 0.450.45

NeNe 0.130.13

MgMg 0.090.09 0.0050.005

SiSi 0.020.02 0.300.30 0.400.40

SS 0.200.20 0.250.25

ArAr 0.0250.025 0.060.06

CaCa 0.020.02 0.050.05

FeFe 0.200.20 0.700.70

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 88

Overturning Our View of Cas AOverturning Our View of Cas A

Hughes, Rakowski, Burrows, and Slane 2000, ApJL, 528, L109.

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 99

Cas A - Doppler Imaging by Cas A - Doppler Imaging by XMMXMM

Similar velocity structures Similar velocity structures in different linesin different lines– SE knots blueshiftedSE knots blueshifted– N knots redshiftedN knots redshifted– Tight correlation between Tight correlation between

Si and S velocitiesSi and S velocities Fe Fe

– Note velocity distribution in Note velocity distribution in NN

– Extends to more positive Extends to more positive velocities than Si or Svelocities than Si or S

Willingale et al 2002, A&A, 381, 1039

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1010

Cas A – 3D Ejecta ModelCas A – 3D Ejecta Model

Red: Si K

Green: S K

Blue: Fe K

Circle: Main shock

“Plane of the sky” “Rotated”

Fe-rich ejecta lies outside Si/S-rich ejecta

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1111

N63AN63A Middle-aged SNRMiddle-aged SNR

– 34” (8.2 pc) in radius34” (8.2 pc) in radius– 2000-5000 yrs old2000-5000 yrs old– 22ndnd brightest LMC SNR brightest LMC SNR

““Crescent”-shaped featuresCrescent”-shaped features– Similar to features in VelaSimilar to features in Vela– Clumps of high speed Clumps of high speed

ejectaejecta– Not ejecta dominatedNot ejecta dominated

Triangular hole Triangular hole – X-ray absorptionX-ray absorption– Approx. 450 solar mass Approx. 450 solar mass

cloudcloud– On near sideOn near side

No PSR or PWNNo PSR or PWN– LLXX < 4x10 < 4x103434 erg s erg s-1-1Warren, Hughes, & Slane, ApJ, in press (20 Jan

2003)

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1212

DEM L71DEM L71 Middle-aged SNRMiddle-aged SNR

– 36” (8.7 pc) in radius36” (8.7 pc) in radius– 4,000 yrs old4,000 yrs old

Rims: LMC compositionRims: LMC composition Core: [Fe]/[O] > 5 times solarCore: [Fe]/[O] > 5 times solar Ejecta mass: 1.5 MEjecta mass: 1.5 Msunsun

Hughes, Ghavamian, Rakowski, & Slane 2003, ApJ, 582, L95

SN Ia ejecta

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1313

N49BN49B Middle-aged SNRMiddle-aged SNR

– 80” (19 pc) in radius80” (19 pc) in radius– 5000-10,000 yrs old5000-10,000 yrs old

Bright and faint rimsBright and faint rims– LMC compositionLMC composition– ISM density varies by x10ISM density varies by x10

EjectaEjecta– Revealed by equivalent-width Revealed by equivalent-width

mapsmaps– Mg & Si rich, no strong O or NeMg & Si rich, no strong O or Ne

Park, Hughes, Slane, Burrows, Garmire, & Nousek 2003, ApJ, in prep.

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1414

SNR 0103-72.6SNR 0103-72.6 Middle-aged SNRMiddle-aged SNR

– 87” (25 pc) in radius87” (25 pc) in radius– >10,000 yrs old (?)>10,000 yrs old (?)

Circular rimCircular rim– SMC compositionSMC composition

Central bright regionCentral bright region– O, Ne, Mg, Si-rich ejectaO, Ne, Mg, Si-rich ejecta– No Fe enhancementNo Fe enhancement

Park, et al 2003, ApJ, in prep.

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1515

DEM L71: Shock PhysicsDEM L71: Shock PhysicsNonradiative Balmer-dominated shockMeasure post-shock proton temperature

X-ray emission from thermal bremsstralungMeasure post-shock electron temperature

H X-ray

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1616

Constraining the Electron Constraining the Electron TemperatureTemperature

Fit plasma shock models to 3 Fit plasma shock models to 3 spatial zones to follow evolution spatial zones to follow evolution of Tof Tee

Study 5 azimuthal regions with Study 5 azimuthal regions with sufficient Chandra statistics and sufficient Chandra statistics and broad Hbroad H component component

Available data cannot constrain TAvailable data cannot constrain Te e

gradientsgradients

Rakowski, Ghavamian, & Hughes 2003, ApJ, submitted

Data do determine mean Te

Suggest partial to compete temperature equilibration

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1717

Nonradiative Balmer ShocksNonradiative Balmer Shocks Nonradiative means that a radiative Nonradiative means that a radiative

(cooling) zone does not form(cooling) zone does not form Low density (partially neutral) gasLow density (partially neutral) gas High velocity shocksHigh velocity shocks Narrow component: cold H I overrun Narrow component: cold H I overrun

by shock, collisionally excitedby shock, collisionally excited Broad component: hot postshock Broad component: hot postshock

protons that charge exchange with protons that charge exchange with cold H Icold H I

Ghavamian, Rakowski, Hughes, and Williams 2003, ApJ, submitted.

Width of broad component yields post shock proton temperature

(Chevalier & Raymond 1978; Chevalier, Kirshner, & Raymond 1980)

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1818

Results on TResults on Tee/T/Tp p from DEM L71from DEM L71 Shows trend: higher equilibration for slower shocksShows trend: higher equilibration for slower shocks X-ray/HX-ray/H results consistent with other purely H results consistent with other purely H ones ones

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1919

Future DirectionsFuture Directions

X-ray expansion (proper X-ray expansion (proper motion)motion)– Cas A: doneCas A: done– SN1006, Tycho: this yearSN1006, Tycho: this year– Magellanic Cloud SNRs: in a Magellanic Cloud SNRs: in a

few yearsfew years Ejecta census in LMC/SMC Ejecta census in LMC/SMC

SNRsSNRs– Probe the “Life Cycle of Probe the “Life Cycle of

Matter”Matter” Longer observations of PWNLonger observations of PWN

– Explore range of dynamical Explore range of dynamical variabilityvariability

More studies of shock physicsMore studies of shock physics– Explore variety of high Mach-Explore variety of high Mach-

number shocksnumber shocks

January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 2020

The EndThe End