1. Hot Relics in GRB Photosphere and GeV Photon Delay Kunihito Ioka (KEK)

2. Very High Lorentz Factor (VHLF)  max can be up to ~10 6 (>  max,conv ~10 3 ) Internal Shock Synchrotron ⇒ Power-law component over >7 decades c t delay ~ Baryon Load Radius ~ Progenitor Radius ~ 10 10 cm Neutrino – GeV  Anti-Correlation

3. Abdo+ 09 Ohno’s talk MeV GeV GeV onset delay  →e + e - ⇒  >10 3 ~1 sec

4. Abdo+ 09 Ohno’s talk GRB 090902B GRB 090510 Band component + Power Law Band ~ Black body-like ⇒ Photosphere emission GeV keV Hurley+94 Gonzaletz+03

5. Photo- sphere Internal Shock External Shock keVMeVGeV Toma, Wu & Meszaros Kumar & Barniol Duran 09 Ghisellini+09, Wang+09 Corsi+09, Gao+10 Variable Long-lived

6. L∝T2L∝T2 L∝T4L∝T4 Yonetoku+KI 03 [Ghirlanda’s talk] A Distance Indicator

7. ln r r0r0 rbrb  r sh r ph T obs mm For Yonetoku Rel. Rees & Meszaros 05 Thompson+ 07 Ghisellini+ 07 Ryde & Pe’er 09 KI+07

8. Radiation in Comoving Proton Energy Density after Shock pp collision thickpp collision thin Accelerated to Very High Radiation Dominated ~ Hot Relics in Cosmology

9.  max ~10 3 Meszaros & Rees Shemi & Piran Paczynski Goodman Baryon-LessBaryon-Rich

10.  max ~10 6 ! KI in prep. Baryon-LessBaryon-Rich

11. KI in prep.

12. Toma+10  ~10 3

13. GRB 090926 Break?? A target for CTA Very High Lorentz Factor (VHLF) case Wang+ 09 Piran & Nakar 10 Barniol Duran & Kumar 10 KI in prep.

14. pp Collision Thick ⇒ Thin [Baryon-rich ⇒ Barion-less]

15. Time MeV  GeV  TeV Time pp thin pp thick pp→  →  ~  m 2 m  c 2 >0.1TeV TeV  – GeV  Anti-Correlation Baryon-less Baryon-rich

16. Very High Lorentz Factor (VHLF)  max can be up to ~10 6 (>  max,conv ~10 3 ) Internal Shock Synchrotron ⇒ Power-law component over >7 decades c t delay ~ [r m =r pp ~L -1/5 ] ~ R star ~ 10 10 cm Neutrino – GeV  Anti-Correlation

17. Coasting  c  m  Mass=E r  r /  m 2 ＜１０ −8 M  （ available at R star ) Energy Momentum Yonetoku Relation Before dissipation, rela. matter E ~ radiation E