Georg Raffelt- Physics Opportunities with Supernova Neutrinos

8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos

http://slidepdf.com/reader/full/georg-raffelt-physics-opportunities-with-supernova-neutrinos 1/65

Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily

Crab NebulaCrab Nebula

Neutrinos in Cosmology, Astro, Particle & Nuclear PhysicsNeutrinos in Cosmology, Astro, Particle & Nuclear Physics

1616 24 September 2009, Erice, Sicily24 September 2009, Erice, Sicily

Physics Opportunit ies withPhysics Opportunit ies with

Supernova NeutrinosSupernova NeutrinosGeorg Raffelt, MaxGeorg Raffelt, Max--PlanckPlanck--Inst itut für PhysikInst itut für Physik,, MünchenMünchen




HeliumHelium--burning starburning star

HeliumHelium

BurningBurning

HydrogenHydrogen

BurningBurning

MainMain--sequence starsequence star

Hydrogen BurningHydrogen Burning

Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion




HeliumHelium--burning starburning star

HeliumHelium

BurningBurning

HydrogenHydrogen

BurningBurning

MainMain--sequence starsequence star

Hydrogen BurningHydrogen Burning

Onion structureOnion structure

Degenerat e i ron core:Degenerat e i ron cor e:

≈≈ 101099 g cmg cm −−33

TT ≈≈ 10101010 KK

MMFeFe ≈≈ 1.5 M1.5 MsunsunRRFeFe ≈≈ 8000 km8000 km

Collapse (implosion)Collapse (implosion)





Collapse (implosion)Collapse (implosion)ExplosionExplosionNewborn Neut ron StarNewborn Neut ron Star

~ 50 km~ 50 km

ProtoProto -- Neut ron St arNeut ron St ar

nucnuc 33 10101414 g cmg cm −−33

TT 30 MeV30 MeV

NeutrinoNeutrinoCoolingCooling





Newborn Neut ron StarNewborn Neut ron Star

~ 50 km~ 50 km

ProtoProto -- Neut ron St arNeut ron St ar

nucnuc 33 10101414 g cmg cm −−33

TT 30 MeV30 MeV

NeutrinoNeutrinoCoolingCooling

Gravit at ional binding energyGravi t at ional binding energy

EEbb ≈≈ 33 10105353 ergerg ≈≈ 17% M17% MSUNSUN cc 22

Thi s show s up asThis shows up as

99% Neut r inos99% Neut r inos

1% Kinet ic ener gy of exp losion1% Kinet ic ener gy of exp losion

(1% of t hi s in t o cosm ic rays)(1% of t hi s in t o cosm ic rays)

0. 01% Phot ons, out shine host galaxy0. 01% Phot ons, out shine host galaxy

Neut r ino lum inosi t yNeut r ino lum inosi t y

LL ≈≈ 33 10105353 erg / 3 secerg / 3 sec

≈≈ 33 10101919 LLSUNSUN

While i t last s, out shines t he ent i r eWhi le i t last s, out shines t he ent i r evisib l e univer sevisib l e univer se



http://slidepdf.com/reader/full/georg-raffelt-physics-opportunities-with-supernova-neutrinos 6/65Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily

Diffuse Supernova Neutrino Background (DSNB)Diffuse Supernova Neutrino Background (DSNB)

Supernova rat e approxim at elySupernova rat e appr oxim at ely

1 SN / 101 SN / 101010 LLSun,BSun,B / 100 years / 100 years

LLsun,Bsun,B == 0. 54 L0. 54 Lsunsun == 22 10103333 er g/ ser g/ s

EEνν ~ 3~ 3 10105353 erg per coreerg per core -- collapsecollapse

CoreCore -- col lapse neut r i no lum inosi t y ofcol lapse neut r i no lum inosi t y of

t ypical galaxy comparable t o phot ont ypical galaxy comparable t o phot on

lum inosi t y ( f r om nuclear burning)lum inosi t y ( f r om nuclear burning)

CoreCore -- col lapse rat e som ew hat largercol lapse rat e somew hat larger

in t he past . Est im at ed pr esentin t he past . Est im at ed pr esent -- dayday

f lux ~ 10 cmf lux ~ 10 cm −−22 ss−−11ee

Beacom & Vagins, hepBeacom & Vagins, hep -- ph/ 0309300ph/ 0309300[ Phys. Rev. Let t . , 93: 171101, 2004][ Phys. Rev. Let t . , 93: 171101, 2004]

Pushing t he boundari es of neut r i noPushing t he boundari es of neut r i no

ast ronom y t o cosm ological dist ancesast ronom y t o cosm ological dist ances



Realistic DSNB EstimateRealistic DSNB Estimate

Horiuchi, Beacom & Dwek, arXiv:0812.3157v3Horiuchi, Beacom & Dwek, arXiv:0812.3157v3



SanduleakSanduleak 69 20269 202

Large Magel l anic CloudLarge Magel lanic CloudDist ance 50 kpcDist ance 50 kpc

(160. 000 l i ght years)(160. 000 l i ght years)

Tarant ula NebulaTarant ula Nebula



SanduleakSanduleak 69 20269 202

Large Magel l anic CloudLarge Magel lanic CloudDist ance 50 kpcDist ance 50 kpc

(160. 000 l i ght years)(160. 000 l i ght years)

Tarant ula NebulaTarant ula Nebula

Supernova 1987ASupernova 1987A

23 February 198723 February 1987

N i Si l f S 1987AN t i Si l f S 1987A



Neut r ino Signal of Supernova 1987ANeut r ino Signal of Supernova 1987A

Wit hin c lock uncer t a int ies,Wit h in c lock uncer t a int ies,signals are cont em por aneoussignals are cont em poraneous

KamiokandeKamiokande -- II (Japan)II (Japan)Water Cherenkov detectorWat er Cherenkov det ect or2140 t ons2140 t onsClock uncer t a int yClock uncer t a int y 1 mi n1 mi n

Irv ineIrv ine-- MichiganMichigan -- Brookhaven (US)Brookhaven (US)Water Cherenkov detectorWater Cherenkov detector6800 t ons6800 t onsClock uncer t a int yClock uncer t a int y 50 m s50 m s

Baksan Scinti l lator TelescopeBaksan Scinti l lator Telescope(Soviet Union) , 200 t ons(Soviet Union) , 200 t onsRandom event c lust er ~ 0. 7/ dayRandom event c lust er ~ 0. 7/ dayClock uncer t a int yClock uncer t a int y +2/ +2/ -- 54 s54 s

2002 Ph i N b l P i f N t i A t2002 Ph i N b l P i f N t i A t



2002 Physics Nobel Prize for Neut r ino Ast ronomy2002 Physics Nobel Prize for Neut r ino Ast ronomy

Ray Davi s Jr .Ray Davi s Jr .

(1914(1914 −− 2006)2006)Masat oshi Koshi baMasat oshi Koshi ba

(*1926)(*1926)

“ f or p ioneer ing cont r ibut ions t o ast rophysics, in“ f or p ioneer ing cont r ibut ions t o ast rophysics, inpar t icu lar for t he det ect ion of cosm ic neut r inos”par t icu lar for t he det ect ion of cosm ic neut r inos”

G & S h b Ph R 58 1117 (1940)G & S h b Ph R 58 1117 (1940)



Gamow & Schoenberg, Phys. Rev. 58:1117 (1940)Gamow & Schoenberg, Phys. Rev. 58:1117 (1940)

Large Detectors for S perno a Ne trinosLarge Detectors for Supernova Neutrinos



Large Detectors for Supernova NeutrinosLarge Detectors for Supernova Neutrinos

SuperSuper --Kamiokande (10Kamiokande (1044))

KamLAND (400)KamLAND (400)MiniBooNEMiniBooNE

(200)(200)

In br acket s event sIn br acket s event s

f or a “ f iduc ia l SN”f or a “ f iduc ia l SN”at dist ance 10 kpcat dist ance 10 kpc

LVD (400)LVD (400)

Borexino (100)Borexino (100)

IceCube (10IceCube (1066))

BaksanBaksan

(100)(100)

Current and NearCurrent and Near Future SN Neutr ino DetectorsFuture SN Neutr ino Detectors



Current and NearCurrent and Near --Future SN Neutr ino DetectorsFuture SN Neutr ino Detectors

Detector Type Locat ion Mass

(kton)

Events

@8 kpc

Status

Super -K Wat er Japan 32 8000 Running (SK IV)

LVD Scint i l l at or It al y 1 300 Running

Kam LAND Scint i l l at or Japan 1 300 RunningBorexino Scint i l l at or It al y 0. 3 100 Running

IceCube Ice Sout h Pole 0. 4/ PMT 1 m i l l ion Running

Baksan Scint i l l at or Russia 0. 33 50 Running

Mini -BOONE Scint i l l at or USA 0. 7 200 Running

HALO Lead Canada 0. 076 85 Under

construct ion

Icarus Liquid argon It al y 0. 6 230 Alm ost ready

NO A Scint i l l at or USA 15 3000 Const ruct ion

star ted

SNO+ Scint i l l at or Canada 1 300 Funded

Adapt ed f rom Kat e Scholb erg, TAUP 2009Adapt ed f rom Kat e Scholberg, TAUP 2009

SuperSuper Kamiokande Neutrino DetectorKamiokande Neutrino Detector



SuperSuper --Kamiokande Neutrino DetectorKamiokande Neutrino Detector

Simulated Supernova Burst in SuperSimulated Supernova Burst in Super KamiokandeKamiokande




Simulated Supernova Burst in SuperSimulated Supernova Burst in Super --KamiokandeKamiokande

Movie by C. Li t t le, includ ing wor k by S. Farrel l & B. Reed,Movie by C. Li t t le, includ ing wor k by S. Farrel l & B. Reed,

(Kat e Scholb erg’ s group at Duke Univer sit y)(Kat e Scholb erg’ s group at Duke Univer sit y)h t t p : / / snews.bn l . gov/ snmovie.h t m lh t t p : / / snews.bn l . gov/ snmovie.h t m l

IceCube Neut r ino Telescope at the South PoleIceCube Neut r ino Telescope at the South Pole




IceCube Neut r ino Telescope at the South PoleIceCube Neut r ino Telescope at the South Pole

•• 1 km1 km 33 ant arc t ic ice, inst rument edant arc t ic ice, inst rument ed

w i t h 4800 phot omul t ip l ie rsw i t h 4800 phot omul t ip l ie rs•• 59 of 80 st r i ngs inst al l ed (2009)59 of 80 st r i ngs inst al l ed (2009)

•• Comp let ion unt i l 2011 f oreseenComp let ion unt i l 2011 f oreseen

IceCube as a Supernova Neut r ino DetectorIceCube as a Supernova Neut r ino Detector




IceCube as a Supernova Neut r ino DetectorIceCube as a Supernova Neut r ino Detector

Each opt ical m odul e (OM) pi cks upEach opt ical m odul e (OM) pi cks up

Cherenkov l ight f rom i t s neighborhood.Cherenkov l ight f rom i t s neighborhood.SN appears as “ corr el at ed noise” .SN appears as “ corr el at ed noise” .

•• About 300About 300

CherenkovCherenkovphotonsphotons

per OMper OM

f rom a SNf rom a SN

at 10 kpcat 10 kpc

•• NoiseNoise

per OMper OM

~280 Hz~280 Hz

•• Tot a l ofTot a l of

4800 OMs4800 OMs

foreseenforeseenin IceCubein IceCube

IceCube SN signal at 10 kpc, basedIceCube SN signal at 10 kpc, based

on a numer ical Liverm ore m odelon a numer ical Liverm ore m odel[ Dighe, Kei l & Raf f e l t , hep[ Dighe, Kei l & Raf f e l t , hep-- ph/ 0303210]ph/ 0303210]

Method f irst discussed byMet hod f ir st di scussed by

•• Pryor , Roos & Webst er ,Pryor , Roos & Webst er ,

ApJ 329:355 (1988)ApJ 329:355 (1988)

•• HalzenHalzen ,, JacobsenJacobsen && ZasZasastroastro -- ph/ 9512080ph/ 9512080

Galactic Supernova Distance DistributionGalactic Supernova Distance Distribution




Galactic Supernova Distance DistributionGalactic Supernova Distance Distribution

Mirizzi,Mir izzi,

Raf fe l t ,Raf fe l t ,Serpico,Serpico,

astroastro -- phph

06043000604300

Average dist ance 10. 7 kpc, rm s di sper sion 4. 9 kpcAverage dist ance 10. 7 kpc, rm s di sper sion 4. 9 kpc(11.9 kpc and 6.0 kpc f or SN Ia dist r i but ion)(11. 9 kpc and 6. 0 kpc f or SN Ia dist r i but ion)

The Red Supergiant Betelgeuse (Alpha Orionis)The Red Supergiant Betelgeuse (Alpha Orionis)




The Red Supergiant Betelgeuse (Alpha Orionis)The Red Supergiant Betelgeuse (Alpha Orionis)

First resolvedFirst resolved

im age of a st arim age of a st arot her t han Sunot her t han Sun

DistanceDistance

(Hipparcos)(Hipparcos)

130 pc (425 lyr )130 pc (425 lyr )

If Bet el geuse goes Super nova:If Bet el geuse goes Super nova:

•• 66 101077 neut r i no event s in Superneut r i no event s in Super -- KamiokandeKamiokande

•• 2. 42. 4 101033 neut ron event s per day f rom Si l iconneut ron event s per d ay f rom Si l icon -- bur ning phasebur ning phase

( f ew days w arning! ) , need neut ron t agging( f ew days w arning! ) , need neut ron t agging[ Odr zywol ek, Misiaszek & Kut schera, ast ro[ Odr zywolek , Misiaszek & Kut schera, ast ro -- ph/ 0311012]ph/ 0311012]

Local Group of GalaxiesLocal Group of Galaxies




Local Group of GalaxiesLocal Group of Galaxies

Current best neut r ino det ect orssensi t ive out t o f ew 100 kpc

With megatonne class (30 x SK)60 events from Andromeda

Next Generat ion LargeNext Generat ion Large--Scale Detector ConceptsScale Detector Concepts




Next Generat ion LargeNext Generat ion Large Scale Detector ConceptsScale Detector Concepts

Memphys

Hyper-K

DUSEL

LBNE

MegatonMegaton--scalescalewater Cherenkovwater Cherenkov

55 100 kton100 kton

liquid Argonliquid Argon

100 kton scale100 kton scalescintillatorscintillator

LENALENA

HanoHanoHanoHano

Looking forwardLooking forward




Looking forwardg

Galactic Supernova RateGalactic Supernova Rate

CoreCore--Collapse SN Rate in the Milky WayCollapse SN Rate in the Milky Way




p y yp y y

Gamm a rays f romGam m a rays f rom2626Al (Mil ky Way)Al (Mil ky Way)

Hist or ical galact icHist or ical galact ic

SNe (al l t ypes)SNe (al l t ypes)

SN st at i st ics inSN st at i st ics in

ext ernal galaxiesext ernal galaxies

No galact ic neut r i noNo galact ic neut r i no

bur st since 1980bur st since 1980

CoreCore -- col l apse SNe per cent urycollapse SNe per century00 11 22 33 44 55 66 77 88 99 1010

van den Bergh & McClure (1994)van den Bergh & McClure (1994)

Cappel l aro & Tur at t o (2000)Cappel l aro & Turat t o (2000)

Diehl et al . (2006)Diehl et al . (2006)

Tam m ann et al . (1994)Tam m ann et al . (1994)

St rom (1994)St rom (1994)

9090 %% CL (25 y obserser vat ion )CL (25 y obserser vat ion ) Alekseev et al. (1993)Alekseev et al. (1993)

Ref er ences: van den Ber gh & McClu re, ApJ 425 (1994) 205. Cappel lRef er ences: van den Ber gh & McClu re, ApJ 425 (1994) 205. Cappel l aro & Tura t t o , ast roaro & Tura t t o , ast ro --

ph/ 0012455. Diehl et a l . , Nat ure 439 (2006) 45. St rom , Ast ron. Aph/ 0012455. Diehl et a l . , Nat ure 439 (2006) 45. St rom , Ast ron. Ast rophys. 288 (1994) L1.st rophys. 288 (1994) L1.Tamm ann et al. , ApJ 92 (1994) 487. Alek seev et al. , JETP 77 (199Tamm ann et al. , ApJ 92 (1994) 487. Alek seev et al. , JETP 77 (1993) 339 and m y updat e.3) 339 and m y updat e.

Observed SNe in the Local Universe (Past Decade)Observed SNe in the Local Universe (Past Decade)




( )( )

Kist lerKist ler ,, YükselYüksel ,, AndoAndo ,, BeacomBeacom && SuzukiSuzuki , arXiv: 0810. 1959, arXiv: 0810. 1959

Stat ist icalStat ist ical

Predic t ionPredic t ion

High and Low Supernova Rates in Nearby GalaxiesHigh and Low Supernova Rates in Nearby Galaxies




g p yg p y

M31 (Andromeda)M31 (Andr om eda)

D = 780 kpcD = 780 kpc

Last Obser ved Super nova: 1885ALast Obser ved Super nova: 1885A

NGC 6946NGC 6946

D = (5. 5 ± 1) MpcD = (5.5 ± 1) Mpc

Obser ved Super novae:Obser ved Super novae:

1917A,1917A, 1939C,1939C, 1948B,1948B, 1968D,1968D, 1969P,1969P,1980K,1980K, 2002hh,2002hh, 2004et,2004et, 2008S2008S

SSuperuperNNovaova EEarlyarly WWarningarning SSystem (SNEWS)ystem (SNEWS)




p y g y ( )

Neut r i no observat ion can aler t ast ronom ersNeut r i no observat ion can aler t ast ronom erssever al hour s in advance t o a supe rnova.sever al hours in advance t o a supernova.

CoincidenceCoincidence

ServerServer

@ BNL@ BNL

SuperSuper -- KK

AlertAlert

Ot her s ?Ot her s ?

LVDLVD

IceCubeIceCube

Super nova 1987ASuper nova 1987A

Earl y Light Cur veEarl y Light Cur ve http://snews.bnl.gov





Probing Supernova PhysicsProbing Supernova Physics

Delayed ExplosionDelayed Explosion




Wil son, Proc. Univ. I l l i nois Meet ing on Num . Ast rophys. (1982)Wil son, Proc. Univ. I l l i nois Meet ing on Num . Ast rophys. (1982)Bet he & Wil son, ApJ 295 (1985) 14Bet he & Wil son, ApJ 295 (1985) 14

Standing Accretion Shock Instability (SASI)Standing Accretion Shock Instability (SASI)




Mezzacappa et al . , h t t p : / / ww w. phy.o rnl . gov/ t si / pages/ simu lat ionsMezzacappa et al . , h t t p : / / ww w. phy.o rnl . gov/ t si / pages/ simu lat ions. h t m l. h t m l

Luminosity Variat ion Detectable in Neutr inos?Luminosity Variat ion Detectable in Neutr inos?




Marek, Janka & MMarek, Janka & Müü l l er , arXiv: 0808. 4136l l er , arXiv: 0808. 4136

Hemispheric averagePolar direct ion

Neut r i no event s in 10 m s bins f orNeut r i no event s in 10 m s bins f or

SN (10 kpc) dur ing accre t ion phase:SN (10 kpc) dur ing accre t ion p hase:

•• SuperSuper -- K 70 1K 70 1σσ ~ 10%~ 10%

•• 30 x Super30 x Super -- K 2K 2××101033 11σσ ~~ 2%2%

•• IceCubeIceCube 11××101044 11σσ ~~ 1%1%

Det ect ing t he spect rum of l umi nosi t yDet ect ing t he spect rum of l umi nosi t y

variat ions canvariat ions can

•• Det ect SASI inst abi l i t y in neut r i nosDet ect SASI inst abi l i t y in neut r i nos

•• Provide equat ionProvide equat ion -- ofof -- s tatestate

in fo rmat ionin fo rmat ion

Fourier Transform of Luminosity VariationFourier Transform of Luminosity Variation




Marek, Janka & MMarek, Janka & Müü l l er , arXiv: 0808. 4136l l er , arXiv: 0808. 4136

ApproximateApproximate

level oflevel of

Poi sson no isePoi sson no ise

in IceCubein IceCube

f or a SN atf or a SN at

10 kpc10 kpc

Hemispheric

average

Polar direction

Detectab i l i t yDetec tab i l i t yt o be st udiedt o be st udied

in more deta i lin more deta i l

(Lund, Marek,(Lund, Marek,

Lunardini ,Lunardini ,Janka, Raffel t ,Janka, Raffel t ,

Work inWork in

progress)progress)

Neutrino Mass and Resolution of Time VariationsNeutrino Mass and Resolution of Time Variations




Signal di sper sion f or Next Nearb y SNSignal di sper sion f or Next Nearby SN

22

eV1

m

E

MeV10

kpc10

Dm s1.5t

⎟

⎟ ⎞

⎜

⎜

⎝

⎛

⎟

⎟ ⎞

⎜

⎜

⎝

⎛

⎟

⎟ ⎞

⎜

⎜

⎝

⎛ =

22

eV1

m

E

MeV10

kpc10

Dm s1.5t

⎟

⎟ ⎞

⎜

⎜

⎝

⎛

⎟

⎟ ⎞

⎜

⎜

⎝

⎛

⎟

⎟ ⎞

⎜

⎜

⎝

⎛ =

•• IceCube bi nning of dat a: 1.64 m s in each OMIceCube b inni ng of dat a: 1.64 m s in each OM

•• Laborat ory neut r ino m ass l im i t : 2 .2 eVLaborat ory neut r ino m ass l im i t : 2 .2 eV

•• Cosmological l imitCosmological l imit ΣΣmm νν < 0. 6 eV, so indi vidual m ass l im it 0.2 eV< 0. 6 eV, so indi vidual m ass l i m it 0. 2 eV

•• KATRIN sensit ivi t y r oughly 0. 2 eVKATRIN sensit ivi t y r oughly 0. 2 eV

For SN signal int erpr et at ion of f ast t im e var i at ions, i t is im poFor SN signal int erpr et at ion of f ast t im e var i at ions, i t is im po r t an t t o haver t an t t o havet he cosm ological l im i t and f ut ure KATRIN m easurem ent / l im i tt he cosm ological l im i t and f ut ure KATRIN m easurem ent / l im i t

Supernova neutr ino af icionadosSupernova neutr ino af icionadosare new customers for KATRIN results!are new customers for KATRIN results!

Gravitational Waves from CoreGravitational Waves from Core--Collapse SupernovaeCollapse Supernovae




MMüü ll er , Ramp p, Buras, Janka, & Shoem aker,l l er , Ramp p, Buras, Janka, & Shoem aker,

“ Toward s gravi t at ional w ave signals f rom“ Toward s gravi t at ional w ave signals f rom

real ist ic core col lapse super nova m odel s, ”real ist ic core col lapse super nova m odel s, ”

astroastro -- ph/ 0309833ph/ 0309833

The gravi tat ionalThe gravi tat ional -- w ave signal f rom convect ionw ave signal f rom convect ionis a gener ic and domi nat ing f eat ureis a gener ic and domi nat ing f eat ure

BounceBounce

Convect ionConvect ion

Asym m et r i c neut r i no emi ssionAsym m et r i c neut r i no emi ssion

Neut rino Emission Around Bounce TimeNeut rino Emission Around Bounce Time




Dif f erent MassDif f erent Mass Neut r i no Tr ansportNeut r i no Tr ansport Nuclear EoSNuclear EoS

KachelriessKachelriess,,TomàsTomàs,, BurasBuras,,

JankaJanka,, MarekMarek

&& RamppRampp ,,

astroastro -- phph / 0412082 / 0412082

PromptPrompt

Neutronizat ionNeutronizat ion

BurstBurst

Millisecond Bounce Time ReconstructionMillisecond Bounce Time Reconstruction




SuperSuper --KamiokandeKamiokande IceCubeIceCube

Halzen & Raff el tHalzen & Raff el t

arXiv:0908.2317arXiv:0908.2317

Onset of neut r inoOnset of neut r ino

emissionemission

PagliaroliPagliaroli ,, VissaniVissani ,, CocciaCoccia && FulgioneFulgione

arXiv:0903.1191arXiv:0903.1191

•• Emission model adapted toEmission model adapted to

measured SN 1987A datameasured SN 1987A data

•• “ Pessimist ic distance” of 20 kpc“ Pessimist ic distance” of 20 kpc

•• Determine bounce t ime to withinDetermine bounce t ime to within

a few tens of millisecondsa few tens of milliseconds10 kpc10 kpc

Do Neut r inos Gravitate?Do Neut r inos Gravitate?




Neut r i nos arr i ve a f ew hours ear l i er t han phot onsNeut r i nos arr i ve a f ew hours ear l i er t han phot ons →→ Early warning (SNEWS)Early warning (SNEWS)SN 1987A: Transi t t im e f or phot ons and neut r i nos equal t o w it hinSN 1987A: Transi t t im e f or phot ons and neut r i nos equal t o w it hin ~ 3h~ 3h

Equal w it hin ~ 1Equal w it hin ~ 1 −− 44 1010 33

Shapiro t im e delay for part ic l es m oving in aShapiro t im e delay for part ic l es m oving in a

gravi t at ional potent ia lgravi t at ional potent ia l

Longo, PRL 60: 173, 1988Longo, PRL 60: 173, 1988

Krauss & Trem aine , PRL 60:176, 1988Krauss & Trem aine , PRL 60:176, 1988

•• Proves dir ect ly t hat neut r i nos respond t o gravi t y in t he usualProves dir ect ly t hat neut r i nos respond t o gravi t y in t he usual w ayw ay

because f or phot ons gravi t at ional l ensing already pr oves t hisbecause f or phot ons gravi t at ional l ensing already pr oves t his pointpoint

•• Cosm ological l i m it sCosm ological l i m it s NN 1 much worse t est of neut r ino grav i t at ion1 much worse t est of neut r ino grav i t at ion

•• Provides l i m it s on paramet ers of cert ain nonProvides l i m it s on paramet ers of cert ain non-- GR t heor ies of gravi t at ionGR t heor ies of gravi t at ion

months51dt) ]t(r[U2t BAShapiro months51dt)]t(r[U2t BAShapiro





Particle Physics BoundsParticle Physics Bounds

The EnergyThe Energy--Loss ArgumentLoss Argument




Neutr inoNeutr ino

spheresphere

NeutrinoNeutrinodiffusiondiffusion

LateLate -- t im e signal m ost sensit ive observablet im e signal m ost sensit ive observable

Em ission of very w eakly int eract ingEm ission of very w eakly int eract ing

par t ic les w ould “ st eal ” energy f rom t hepar t ic les w ould “ st eal ” energy f r om t heneut r i no burst and short en i t .neut r i no burst and short en i t .

(Ear ly neut r i no burst power ed by accret ion,(Early neut r i no burst power ed by accret ion,

not sensit ive t o volum e energy loss. )not sensit ive t o volum e energy loss. )

Volume emissionVolume emission

of novel part iclesof novel part icles

SN 1987A neut r ino signalSN 1987A neu t r ino signal

New LongNew Long--Term Cooling Calculat ionsTerm Cooling Calculat ions




Fischer et al. (Basel Group), arXiv: 0908.1871Fischer et al. (Basel Group), arXiv: 0908.1871





Neutr ino Flavor Oscillat ionsNeutr ino Flavor Oscillat ions

Neut rino Emission Around Bounce TimeNeut rino Emission Around Bounce Time




Dif f erent MassDif f erent Mass Neut ri no TransportNeut r i no Transport Nucl ear EoSNucl ear EoS

KachelriessKachelriess,,TomàsTomàs,, BurasBuras,,

JankaJanka,, MarekMarek

&& RamppRampp ,,

astroastro -- phph / 0412082 / 0412082

PromptPrompt

Neutronizat ionNeutronizat ion

BurstBurst

Flavor Dependence of Neut r ino EmissionFlavor Dependence of Neut r ino Emission




Fischer et al. (Basel Group), arXiv: 0908.1871Fischer et al. (Basel Group), arXiv: 0908.1871

FlavorFlavor --Dependent Neut r ino Fluxes vs. Equat ion of StateDependent Neut r ino Fluxes vs. Equat ion of State




Kit aura, Janka & Hi l lebr andt , “ Explosions of OKit aura, Janka & Hi l lebr andt , “ Explosions of O-- NeNe -- Mg cores, t he CrabMg cor es, t he Crabsuper nova, and subl um inous Type IIsuper nova, and subl um inous Type II -- P supernovae” , ast roP supernovae” , ast ro -- ph/ 0512065ph/ 0512065

Wolf f & Hil lebrandt nuclear EoS (st if f) Lat t imer & Swesty nuclear EoS (soft )

LevelLevel --Crossing Diagram in a SN EnvelopeCrossing Diagram in a SN Envelope




Dighe & Sm ir nov, Ident i f y ing t he neut r i no mass spect rum f rom a sDighe & Sm ir nov, Ident i f y ing t he neut r i no mass spect rum f rom a supernovaupernova

neut r ino burst , ast roneut r ino burst , ast ro -- ph/ 9907423ph/ 9907423

Normal mass hierarchyNormal mass hierarchy Inverted mass hierarchyInverted mass hierarchy

Spect ra Emerging from a SupernovaSpect ra Emerging from a Supernova




Prim ary f luxesPr im ary f luxes

f orf or

f orf or

f orf or

0eF0eF

0eF0eF

0xF0xF

ee

ee

,,, ,,,

Af t er leaving t heAf t er leaving t he

super nova envelope,super nova envelope,

t he f luxes aret he f luxes are

par t ia l ly sw appedpart ia l ly sw apped

0x0e0e F)p1(FpF 0x0e0e F)p1(FpF

0x

0e

0e F)p1(FpF

0x

0e

0e F)p1(FpF

0

e

0

e

0

xx4

1 F4

p1F

4

p1F

4

pp2F

0

e

0

e

0

xx4

1 F4

p1F

4

p1F

4

pp2F

NormalNormal

Inver tedInver ted

sinsin 22 (2(2 1313 ))

1010−−55

1010−−33

AnyAny

Mass orde r ingMass orde r ing

sinsin 22 (( 1212 ))

00 coscos22 (( 1212 ))

sinsin 22 (( 1212 )) coscos22 (( 1212 ))

00

CaseCase

AA

BB

CC

Survival pr obabi l i t ySurvival pr obabi l i t y

)f or(pe

)f or(p e )f or(pe

)f or(p e

Collective Effects in Neutrino Flavor OscillationsCollective Effects in Neutrino Flavor Oscillations




Coll apsed super nova core or accret ion t orus ofColl apsed super nova core or accret ion t orus of

m erging neut ron st ars:m erging neut ron st ars:

•• Neut r i no f l ux very dense: Up t o 10Neut r i no f l ux very dense: Up t o 103535 cmcm −−33

•• Neutr inoNeutr ino -- neut r ino int eract ion energyneut r ino int eract ion energy

m uch larger t han vacuum osci l l at ion f r equencym uch larger t han vacuum osci l l at ion f r equency

•• Large “ mat t er ef f ect ” o f neut r inos on eachLarge “ mat t e r e f f ect ” o f neut r inos on eachotherother

•• NonNon -- l inear osc i l l a t ion ef f ect sl inear osc i l l a t ion ef f ect s

•• Assume 80% antiAssume 80% anti -- neut r inosneut r inos

•• Vacuum osci l l at ion f requencyVacuum osci l l at ion f requency

= 0. 3 km= 0. 3 km −−11

•• Neutr inoNeutr ino -- neut r ino in t erac t ionneut r ino in t erac t ionenergy at nu spher e (r = 10 km )energy at nu spher e (r = 10 km )

= 0. 3= 0. 3 101055 kmkm −−11

•• Fal ls of f appr oxim at ely asFal ls of f appr oxim at ely as rr−−44

(geomet r ic f lux d i lu t ion and nus(geomet r ic f lux d i lu t ion and nus

becom e more cobecom e more co -- l inear)l inear)

Collective SN Neutrino Oscillations since 2006Collective SN Neutrino Oscillations since 2006




Two seminal papers in 2006 tr iggered a torrent of act ivi t iesDuan, Fuller, Qian, astro-ph/0511275, Duan et al. astro-ph/0606616

Duan, Fuller, Carlson & Qian, ast ro-ph/0608050, 0703776, arXiv:0707.0290,0710.1271. Duan, Fuller & Qian, arXiv:0706.4293, 0801.1363, 0808.2046.

Duan, Fuller & Carlson, arXiv:0803.3650. Duan & Kneller, arXiv:0904.0974.

Hannestad, Raffelt , Sigl & Wong, ast ro-ph/0608695. Balantekin & Pehlivan,ast ro-ph/0607527. Balantekin, Gava & Volpe, arXiv:0710.3112. Gava & Volpe,arXiv:0807.3418. Gava, Kneller, Volpe & McLaughlin, arXiv:0902.0317.

Raffelt & Sigl, hep-ph/0701182. Raffelt & Smirnov, arXiv:0705.1830,

0709.4641. Esteban-Pretel, Pastor, Tomàs, Raffelt & Sigl, arXiv:0706.2498,0712.1137. Esteban-Pretel, Mirizzi, Pastor, Tomàs, Raffelt, Serpico & Sigl,arXiv:0807.0659. Raffelt , arXiv:0810.1407. Fogli , Lisi, Marrone & Mir izzi,arXiv:0707.1998. Fogli, Lisi, Marrone & Tamborra, arXiv:0812.3031,

0907.5115. Lunardini, Müller & Janka, arXiv:0712.3000. Dasgupta & Dighe,arXiv:0712.3798. Dasgupta, Dighe & Mirizzi, arXiv:0802.1481. Dasgupta,Dighe, Mir izzi & Raffelt , arXiv:0801.1660, 0805.3300. Dasgupta, Dighe,Raffelt & Smirnov, arXiv:0904.3542. Sawyer, arXiv:0803.4319.Chakraborty, Choubey, Dasgupta & Kar, arXiv:0805.3131. Blennow, Mir izzi &

Serpico, arXiv:0810.2297. Wei Liao, arXiv:0904.0075, 0904.2855.

General Equat ions of Mot ionGeneral Equat ions of Mot ion




( )]) ,) [ (cos1(

2qdG2],L[G2,

p2Mi pqqqp3

3

FpFp

2

ptrrrrrrrr

v

−−⎮⌡

⌠ ++

⎥⎥⎦

⎤

⎢⎢⎣

⎡+=∂

( )]) ,) [ (cos1(

2qdG2],L[G2,

p2Mi pqqqp3

3

FpFp

2

ptrrrrrrrr

v

−−⎮⌡

⌠ ++

⎥⎥⎦

⎤

⎢⎢⎣

⎡+=∂

( )]) ,) [ (cos1(

2

qdG2],L[G2,

p2

Mi pqqqp3

3

FpFp

2

ptrrrrrrrr

v

−−⎮⌡

⌠ ++

⎥⎥⎦

⎤

⎢⎢⎣

⎡−=∂

( )]) ,) [ (cos1(

2

qdG2],L[G2,

p2

Mi pqqqp3

3

FpFp

2

ptrrrrrrrr

v

−−⎮⌡

⌠ ++

⎥⎥⎦

⎤

⎢⎢⎣

⎡−=∂

Usual m at t e r e f fec t w i t hUsual m at t e r e f fec t w i t h

nn00

0nn0

00nn

L

ee

nn00

0nn0

00nn

L

ee

•• Vacuum osci l lat ionsVacuum osci l lat ions

M is neut r i no m ass m at r i xM is neut r i no m ass m at r i x

•• Not e opposit e sign bet w eenNot e opposit e sign bet w een

neut r inos and ant ineut r inosneut r inos and ant ineut r inos

Nonlinear nuNonlinear nu -- nu ef f ect s are im port antnu ef f ect s are im port ant

w hen nuw hen nu -- nu int eract ion energy exceedsnu int eract ion energy exceeds

t ypical vacuum osci l l a t ion f requencyt ypical vacuum osci l l a t ion f requency(Do no t compare w i t h mat t e r e f fec t ! )(Do no t compare w i t h mat t e r e f fec t ! )

cos1nG2E2

m

F

2

osc

cos1nG2E2

m

F

2

osc

Oscillat ions of Neutr inos plus Ant ineutr inos in a BoxOscillat ions of Neutr inos plus Ant ineutr inos in a Box

m 2m 2




Equal and densit ies, single energy E, w it hEqual and densit ies, single energy E, w it hee eeE2

mnG2

2

F e=>=

E2

mnG2 F e

=>=

P)PP(PBPt ×−+×+=∂ P)PP(PBPt ×−+×+=∂

EqualEqualse l f t ermssel f t erms

P)PP(PBPt ×−+×−=∂ P)PP(PBPt ×−+×−=∂

)( )(

)( )(43421 43421 4 434 421 4 434 421

Opposit e vacuumOpposit e vacuumosci l lat ionsosci l lat ions

==

PP

PP

BB

PP

PP

BB

“ Pendulum in f lavor space”“ Pendulum in f lavor space”•• Invert ed m ass hier archyInvert ed m ass hier archy

→→ Inver t ed pendulumInver t ed pendulum

→→ UnstableUnstable eveneven f orf or smallsmall mix ingmix ing angleangle

•• Norm al m ass hier archyNorm al m ass hier archy→→ SmallSmall -- ampl i tude osc i l la t ionsampl i tude osc i l la t ions

Flavor Conversion in Toy SupernovaFlavor Conversion in Toy Supernova

A 80% i i




Pendular

Oscillations

•• Assume 80% antiAssume 80% anti -- neut r inosneut r inos

•• Vacuum osci l lat ion f requencyVacuum osci l l at ion f requency= 0. 3 km= 0. 3 km −−11

•• Neutr inoNeutr ino -- neut r ino in t erac t ionneut r ino in t erac t ion

energy at nu spher e (r = 10 km)energy at nu spher e (r = 10 km)

= 0. 3= 0. 3 101055 kmkm −−11

•• Fal ls of f appr oxim at ely asFal ls of f appr oxim at ely as rr−−44

(geomet r ic f lux d i lu t ion and nus(geomet r ic f lux d i lu t ion and nus

becom e more cobecom e mor e co-- l inear)l inear)

Decl ine of osc i l l a t ion ampl i t udeDecl ine of osc i l l a t ion ampl i t ude

explained in pendul um analogyexplained in pendul um analogy

by inreasing m oment of iner t iaby inreasing m oment of iner t ia

(Hannest ad, Raff el t , Sigl & Wong(Hannest ad, Raff el t , Sigl & Wongastroastro -- ph/ 0608695)ph/ 0608695)

Spectral Split for Accretion Phase ExampleSpectral Split for Accretion Phase Example




FogliFogli et al . , arXiv: 0707. 1998, 0808. 0807et al . , arXiv: 0707. 1998, 0808. 0807

In i t ial f luxesIn i t ia l f luxes

at nu spher eat nu spher e

Af te rA f te r

co l lec t iveco l lec t ive

t ranst rans

--

fo rmat ionformat ion

For exp lanat ion seeFor exp lanat ion see

Raff el t & Sm ir novRaff el t & Sm ir nov

arXiv:0705.1830arXiv:0705.1830

0709.46410709.4641

Duan, Ful l er,Duan, Ful l er,Carl son & QianCarl son & QianarXiv:0706.4293arXiv:0706.4293

0707.02900707.0290

Mult iple Spectral Splits (CoolingMult iple Spectral Splits (Cooling--Phase Example)Phase Example)




Dasgupt a, Dighe, Raf f elt & Sm ir nov, arXiv: 0904. 3542Dasgupt a, Dighe, Raf f elt & Sm ir nov, arXiv: 0904. 3542

ee

xxee xx

InvertedHierarchy

Normal

Hierarchy

Mult iple Spect ral Splits in t heMult iple Spect ral Splits in t he VariableVariable

Given is t he f lux spect rum f (E) f orGiven is t he f lux spect rum f (E) f or




Dasgupt a, Dighe, Raf f el t & Sm ir nov,Dasgupt a, Dighe, Raf f el t & Sm ir nov,arXiv:0904.3542arXiv:0904.3542

Given is t he f lux spect rum f (E) f orGiven is t he f lux spect rum f (E) f or

each f lavoreach f lavor

UseUse mm 22 / 2E t o l abel m odes / 2E t o l abel m odes

Label ant iLabel ant i -- neut r inos w i t hneut r inos w i t h −−

ant ineut r inos neut r inos

ee

xx

ee

xx

Def ine “ spec t r um” asDef ine “ spect rum” as

)E(f)E(f

)E(f)E(f)(g

ex

xeNeutr inosNeutr inos

Ant ineut r inosAnt ineut r inos

Sw aps devel op around everySw aps deve lop around every

“ posi t ive” spect ra l crossing“ posi t ive” spect ra l crossing

Each sw ap f lanked by t w o spl i t sEach sw ap f lanked by t w o spl i t s

Flavor PendulumFlavor Pendulum

Si l “ i t i ” iSi l “ i t i ” i Si l “ t i ” iSi l “ t i ” i




Dasgupt a, Dighe, Raf f el t & Sm ir nov, arXiv: 0904.3542Dasgupt a, Dighe, Raf f elt & Sm ir nov, arXiv: 0904.3542

For m ovies seeFor m ovies see ht t p : / / ww w. m ppm u. m pg. de/ supernova/ m u l t i sp l i t sh t t p : / / ww w. m ppm u. m pg. de/ supernova/ m u l t i sp l it s

Single “ posi t ive” crossingSingle “ posi t ive” crossing

(pot ent i al energy at a maxim um)(pot ent i al energy at a maxim um)

Single “ negat ive” crossingSingle “ negat ive” crossing

(pot ent i al energy at a min imum )(pot ent i al energy at a min imum )

Decreasing Neut r ino DensityDecreasing Neut r ino Density

Fo r t im es sm al lerFour t im es sm al ler




Cert a in in i t ia l neut r ino densi t yCert a in in i t ia l neut r ino densi t yFour t im es sm al lerFour t im es sm al ler

in i t ia l neut r ino densi t yin i t ial neut r ino densi t y


For movies see ht t p : / / ww w. mppmu.mpg.de / supernova/ mu l t i sp l i t sFor movies see ht t p : / / ww w. mppmu.mpg.de / supernova/ mu l t i sp l i t s

Supernova CoolingSupernova Cooling--Phase ExamplePhase Example




Norm al Hier archyNorm al Hier archy Inverted HierarchyInverted Hierarchy


For movies see ht t p : / / ww w. mppmu.mpg.de / supernova/ mu l t i sp l i t sFor movies see ht t p : / / ww w. mppmu.mpg.de / supernova/ mu l t i sp l i t s

Mult iple Spectral Splits (CoolingMult iple Spectral Splits (Cooling--Phase Example)Phase Example)





ee

xxee xx

InvertedHierarchy

Normal

Hierarchy

Quest ions and Opportunit iesQuest ions and Opportunit ies




SelfSelf -- induced col l ect ive osci l l a t ions occur eveninduced col l ect ive osci l la t ions occur evenf or very sm al l 13f or very sm al l 13-- m ix ing ( inst ab i l i t y ! )m ix ing ( inst ab i l i t y ! )

Do mat t erDo mat t er -- densi t y f luct uat ions have anydensi t y f luct uat ions have anyreal ist ic im pact ?real ist ic im pact ?

Theoret ical underst anding and r o le ofTheor et ical underst anding and r o le of“ m u l t i“ m u l t i -- angle ef f ect s” largely m issingangle ef f ect s” largely m issing

Observat ion of spect ra l spl i t or sw ap indicat ionObservat ion of spect r al spl i t or sw ap indicat ioncan provide signat ure f or m ass hier archycan provid e signat ure f or m ass hier archy

and nont r i v ial neut r i no propagat ion dynam icsand nont r i v ial neut r i no propagat ion dynam ics

Spect ral Split (Accret ionSpect ral Split (Accret ion--Phase Example)Phase Example)




FogliFogli ,, LisiLisi ,, MarroneMarrone & M& Mir izzii r izz i , arXiv: 0707. 1998, arXiv: 0707.1998

In i t ia l f l uxesIn i t ia l f luxes

at neut r inoat neut r ino

spheresphere

Af te rA f te r

co l lec t iveco l lec t ive

t ranst rans--

fo rmat ionformat ion

For exp lanat ion seeFor exp lanat ion see

Raf f e l t & Sm irnovRaff el t & Sm ir nov

arXiv:0705.1830arXiv:0705.1830

0709.46410709.4641

Duan, Ful l er,Duan, Ful l er,Carl son & QianCarl son & QianarXiv:0706.4293arXiv:0706.4293

0707.02900707.0290

Dist inguishing Mixing ScenariosDist inguishing Mixing Scenarios

Survival Probabil i tySurvival Probabil i ty




HierarchyHierarchy sinsin 221313

Survival Probabil i tySurvival Probabil i ty

EarthEarthe f fec t se f fec t s

NormalNormal

Inver tedInver ted1010−−33

1010−−55

coscos221212

NormalNormal

Inver tedInver ted −−

sinsin22

1212

00

sinsin22

1212

00

E < EE < Espli tspl i t E > EE > Espli tspl i t

eeee

00

00

ee

ee

ee

•• Assum ing “ st andard” f lux spect ra l eading t o a single spl i tAssum ing “ st andard” f lux spect ra leading t o a single spl i t•• Probably gener ic f or accret ion phaseProbably gener ic f or accret ion phase

Adapt ed f r omAdapt ed f r om DigheDighe , arXiv: 0809.2977, arXiv: 0809.2977

Mass Hierarchy at Ext remely Small ThetaMass Hierarchy at Ext remely Small Theta--1313

Using Eart h mat t er ef f ect s t o diagnose t ransf orm at ionsUsing Eart h mat t er ef f ect s t o diagnose t ransf orm at ions




Dasgupt a, Dighe & Mir izzi, arXiv: 0802.1481Dasgupt a, Dighe & Mir izzi, arXiv: 0802. 1481

Rat io of spect ra inRat io of spect ra in

t w o w at er Cherenkovt w o w ater Cherenkov

det ect ors (0.4 Mt on) ,det ect ors (0.4 Mt on),

one shadowed b y t heone shadowed b y t he

Ear t h , t he ot her notEar t h , t he ot her not

g gg g

Diagnosing Collective TransformationsDiagnosing Collective Transformations

Assum ing t he m ass ord eri ng is m easured t o be inver t ed in t he labAssum ing t he m ass ord eri ng is m easured t o be inver t ed in t he lab




HierarchyHierarchy sinsin22

1313

survivalsurvival

probabi l i t yprobabi l i t y

NormalNormal

Inver tedInver ted

1010−−33

1010−−55

coscos22

1212

NormalNormal

Inver tedInver ted NoNo

ee EarthEarth

e f fec t se f fec t s

ee survivalsurvival

probabi l i t yprobabi l i t y

ee EarthEarth

e f fec t se f fec t s

ee

00

YesYes

coscos221212

00

coscos221212

NoNo

YesYes

YesYes

Col lect ive Transformat ionsCol lect ive Transformat ions

NoNo YesYes

Assum ing t he m ass ord eri ng is m easured t o be inver t ed in t he labAssum ing t he m ass ord eri ng is m easured t o be inver t ed in t he lab ,,

t he presence or absence of Eart h ef f ect s di st inguishes bet w eent he pr esence or absence of Eart h ef f ect s dist inguishes bet w eent he presence or not of col lect ive t ransf orm at ionst he presence or not of col lect ive t ransf orm at ions





What exact ly will be learnt from the neutr inosWhat exact ly will be learnt from the neutr inos

of the next nearby SN depends a lot on whatof the next nearby SN depends a lot on whatexact ly is observedexact ly is observed





SN neut r inos are powerful ast rophysicalSN neut r inos are powerful ast rophysical

and part icleand part icle--physics messengersphysics messengers

Documents

Georg Raffelt- Physics Opportunities with Supernova Neutrinos