Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily Crab Nebula Crab Nebula Neutrinos in Cosmology, Astro, Particle & Nuclear Physics Neutrinos in Cosmology, Astro, Particle & Nuclear Physics 16 16 24 September 2009, Erice, Sicily 24 September 2009, Erice, Sicily P hys ics O ppor t unities with Physics Opportuni t ies w ith Supernova Neutrinos Supernova Neutrinos Georg Raffelt, Max Georg Raffelt, Max - Planck Planck - Ins t i t ut f ür P hys i k Ins t i t ut f ür P hys i k , München München
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Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
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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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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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)
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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Large Detectors for S perno a Ne trinosLarge Detectors for Supernova Neutrinos
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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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
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Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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 ,
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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)
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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)
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
Looking forwardLooking forward
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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?
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
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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
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Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
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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
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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
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( )]) ,) [ (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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
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 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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
Norm al Hier archyNorm al Hier archy Inverted HierarchyInverted Hierarchy
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 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
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Neutrinos in Cosmology, Astro, Particle & Nuclear Physics, 16 24 September 2009, Eri ce, Sicily
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
Looking forwardLooking forward
8/3/2019 Georg Raffelt- Physics Opportunities with Supernova Neutrinos