Supernova and GRB remnants and their Ge VTe

Supernova and GRB remnants and their Ge. V-Te. V g-ray emission Kunihito Ioka (KEK) Peter Mészáros (IGC, Penn State) 1. GRB/Hypernova remnants ~ Te. V un. ID sources 2. A new mechanism for Te. V g: Radio Isotope decay

Contents Te. V unidentified (Te. V un. ID) sources No counterpart, Origin unknown Gamma-Ray Burst (GRB) GRB-Supernova/Hypernova GRB/Hypernova remnant-Te. V un. ID 1. p 0 decay: Nobs(HNR)~Nobs(SNR) 2. b decay + e-Inverse Compton 3. Radio isotope (RI) decay

Multi-wavelength sky Radio IR Opt X g New wavelength⇒New sources (GRB, pulsar, …)

Increasing Te. V sources “Kifune plot” Jim Hinton, rapporteurtalk, ICRC 2007 Most abundant category: un. ID! No clear counterparts at other wavelengths

HESS Galactic survey

Observed properties Te. V un. ID Disk ⇒ Galactic origin Aha+ 06 Extended

Te. V g-ray Leptonic process Electron acceleration (e with 10 -100 Te. V) Synchrotron⇒X Inverse Compton⇒g Hadronic process Magnetic Field CMB g Inverse Compton (g) Proton acceleration (p with 10 -100 Te. V) pp⇒p 0 decay⇒ 2 g Synchrotron (X) p 0 Nucleus 2 g p+

Koyama+ 05 SNR Bamba+ 03 CR acceleration at SN shock Aha+ 04 Hwang+ 04 Most likely Galactic CR origin Also likely Te. V g sources

Suzaku upper limit X-ray Suzaku⇒Strong X-ray upper limit FTe. V/FX>50 Te. V g ⇒ Leptonic × Hadronic ○ ⇒ Young SNR × Matsumoto+ 07 Bamba+ 07

Old SNR? Yamazaki+ 06 X Te. V In old SNRs, emax, electron is low but p 0 g flux~const ⇒ FTe. V/FX>100 But, Rate~1/100 yr⇒ 103 SNR ⇔ 10 un. ID

GRB = Rare SN Luminosity >msec The most luminous objects ~1051 erg/s Afterglow GRB X Opt Radio ～ 1000 events/yr isotropic ～ 200 ke. V, nonthermal 10 -3 s～ 103 s : Short, Long Redshift SN ~1 day Time

Standard model optically thick gg→e+e- Internal shock SN? ？ ISM G>100 Central Engine 光度 Kinetic energy ↓ Shock dissipation GRB External shock Afterglow 時間

GRB-SN Afterglow Light curve Bloom+(99) Hjorth+(03) Type Ic spectrum ⇒ GRB is associated with SN Ibc

Collapsar Jet breaks out the massive stellar envelope

GRB/Hypernova Hypernove (hyper-energetic SNe) occur more frequently than GRBs Nomoto+ EHN~1052 erg RSN~1/100 yr RHN~1/104 yr RGRB~1/105 yr tage~105 yr ⇒ NHN~10~Nun. ID

Old GRB/HN remnant g-ray Flux for pp→p 0→ 2 g Just by scaling the SNR calculations ~Fun. ID CR energy~1051 erg~10%x 1052 erg Flux: t-independent ⇒ Old ones are dominated ⇒ leptonic emission is weak (low emax, e) ⇒ un. ID Number R~1/104 yr tage~105 yr ⇒ NHN~10~Nun. ID Size

Observed number ratio Observed #(HNR)~Observed #(SNR) ① ~10 times energy ⇒ dmax∝E 1/2 ② Sensitivity to extended sources∝(size)∝d-1 ⇒ dmax∝E ⇒ Volume∝dmax 2∝E 2 Observable SNRs are nearby ⇒ Size is too large?

GRB jet-Cosmic Ray SN shock B Hillas diagram GRB E<Ze. BR Internal shock External shock also accelerate cosmic ray RGRB~1/105 yr ⇒ NGRB~1 but recent obs. suggest RGRB w/ slow jet~1/104 yr~RHN R

GRB remnant (GRBR) Loeb & Perna 98 Wick, Dermer & Atoyan 04 Dermer & Atoyan 06 After non-rela ⇒ Jet→Sphere ⇒ GRBR~SNR hydrodynamically (cf. , R~E 1/5) Metal distribution could be different Ayal & Piran 01

1. 0 p decay HESS J 1301 -631 SNR All Atoyan, Buckley & Krawczynski 06 Relativistic souces ⇒ less particle @ low E ⇒ Low Ge. V & Radio emission

2. b decay – e-IC ep~1016 g 7 e. V pg→np+ tdecay~900 s g (CMB, …) Energy fraction of Te. V g KI, Kobayashi & Mészáros 04

Unique morphology KI, Kobayashi & Mészáros 04 W 49 B SNR Elongated emission outside SNR Less e @ low E Age/Energy dependent profile Dim @Ge. V & radio

Candidate? Aha+ 06

3. Radio isotope (RI) decay 56 Ni ⇐ SN light curve 1998 bw: M(56 Ni)~0. 4 M◉ ~2 Me. V Could be shock-accelerated before decay (by reverse shock? ) No need for target g and matter

SN light & RI decay NS/BH Nomoto+07 56 Ni, 56 Co decay ⇒SN light curve Complete Si burning⇒ 56 Ni Fall back to central BH/NS

Fe(56 Ni) O Woosley & Zhang 07 Mazzali+05

RI decay model 56 Co case 56 Co energy GRB jet OK SNR disappears Energy fraction of Te. V g ~energetic GRB

Spectrum n. Fn tdecay~106 g 6 yr eg~Te. Vg 6 t (2 -p)-1 n Exp. cutoff Already decayed ~Ge. V Now decaying ~Te. V n

RI model spectrum 105 yr Radio p-2 nd e+ X

Auger Fe ? Depth of air shower maximum

Photo-disintegration Murase, KI+08 Wang, Razzaque & Mészáros 07 Ni/Co/Fe can survive photo-disintegration (⇔ Fe UHECR implied by Auger Xmax)

Model identificaion Neutrino p 0 b RI No n (Already decayed) g Morphology

Summary Te. V un. ID sources Dominant in Te. V sky, Origin unknown Old GRB/Hypernova remnant Nobs(HNR)~Nobs(SNR) SNR may be more nearby and extended BH in un. ID? A new mechanism for g-ray production Decay of Accelerated Radio Isotope (RI) No need for target matter or photon