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Gamma-Ray Bursts from Radiation-Dominated Jet?

Gamma-Ray Bursts from Radiation-Dominated Jet?. Kunihito Ioka (KEK). T. Inoue, Asano & KI, arXiv : 1011.6350 KI , arXiv : 1006.3073 Suwa & KI, arXiv : 1009.6001 KI+, in preparation ( arXiv : 1103.5746). Sorry for changing the title to a preliminary study Comments welcome.

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Gamma-Ray Bursts from Radiation-Dominated Jet?

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  1. Gamma-Ray Bursts from Radiation-Dominated Jet? KunihitoIoka (KEK) T. Inoue, Asano & KI, arXiv: 1011.6350 KI, arXiv: 1006.3073 Suwa & KI, arXiv: 1009.6001 KI+, in preparation (arXiv: 1103.5746) Sorry for changing the title to a preliminary study Comments welcome

  2. Baryon Loading G or r/r0 Paczynski, Goodman Meszaros & Rees Shemi & Piran Matter- Dominated G* ~103 Radiation-Dominated Photon-to-Baryon h*~103 h=E/Mc2

  3. Baryon Loading G or r/r0 Compactness Non-thermal IS Synchro. Photosphere Original Paczynski Goodman Beloborodov Vurm, Daigne Medvedev, Ryde, Lundman G* ~103 Except Zhang & Yan 11, KI 10, Tchekhovskoy+ 10, McKinney 10, Gianinnos+ 07 (& others?) Photon-to-Baryon h*~103 ~102 h=E/Mc2

  4. Fermi Revolution GeVg from GRBs GRB 090510 GeV keV MeV Abdo+ 09

  5. Baryon Loading G or r/r0 Fermi limit Omodei Racusin Ghisellini BB Zhang IS Synchro. Photosphere Original Paczynski Goodman G* ~103 Photon-to-Baryon h*~103 h=E/Mc2 But, Hascoet+ 11 Zou+ 10, Aoi+ 10

  6. Baryon Loading G or r/r0 Fermi limit Omodei Racusin Ghisellini BB Zhang IS Synchro. Photosphere Original Paczynski Goodman Fine Tuning? G* ~103 Photon-to-Baryon h*~103 h=E/Mc2

  7. Internal Shock in RD? Time (t) Light path Rapid Shell ⇒ No Internal Shock Slow Shell r0 Space (r)

  8. Confinement External pressure or Magnetic Tchekhovskoy Narayan

  9. Internal Shock in RD? Time (t) Light path ⇒ No Internal Shock r0 Space (r)

  10. Internal Shock in RD! Time (t) Light path r0 Space (r)

  11. Internal Shock in RD! Time (t) All rapid shells can catch-up like IS Light path r/G2 always increases (so trivial) Poynting models r0 Space (r)

  12. Internal Shock of RD Flow 1. Internal Shock is possible for RD outflow 2. Up to a large radius 3. Repeatedly ⇒ Can keep e± up to high G

  13. Cocoon Confinement Pressure balance at Jet head Cocoon-Star Jet-Cocoon ~1/2 for n=3 (Rad. env.) ⇒ Dissipative Aloy+ 00, Lazzati+ 09, Morsony+ 10, Mizuta+ 10

  14. Cocoon Confinement Pressure balance at Jet head Cocoon-Star Jet-Cocoon ~1/2 for n=3 (Rad. env.) ⇒ Dissipative Aloy+ 00, Lazzati+ 09, Morsony+ 10, Mizuta+ 10

  15. Fast Cocoon just escaping from the jet head sideways at the breakout Gfc~Gj(tbreak)~10-30 ⇒ persist aroundthe jet pfc~r-8/3 pj~r-4 ⇒ Confine ⇒ Internal Shock

  16. Shock ⇒ g acceleration ⇒ e± • Photons carries almost all the energy • Shock via Compton (g mediated shock) • Fermi-like acceleration of photons • y-parameter can be of unity • Appreciable energy can go to gg→e± • Outflow can keep e±tT~Dt’shock/t’dyn>1 Budnik+ 10 Blandford & Payne 78 Density or G electron/positron

  17. Turbulence 3D Rela. MHD Thompson 94 Richtmyer-Meshkov turbulence T. Inoue, Asano & KI 11 A small Dn is enough to drive turbulence

  18. Lorentz Factor If e± are kept by internal shocks out to e± photosphere l=2/3 in the last eq. High Lorentz Factor c.f. KI(10) for baryonic case

  19. Extended g-Generation Shocks would continue beyond photosphere Radiation-Dom. Internal Shock Photo- sphere ~GGrel2mec2 GeV MeV

  20. CTA O’Brien Granot S. Inoue • ~20GeV-100TeV • x10 Sensitivity • Dq~1-2 min • FOV~5-10 deg • ~20 s slew (LST) • ~2015 (?) • ~150€ TeVg from GRB or not?

  21. Summary G or r/r0 Fermi limit IS Synchro. Photosphere Original Paczynski Goodman Fine Tuning? G* ~103 Photon-to-Baryon h*~103 h=E/Mc2

  22. Summary G or r/r0 Unexplored Frontier? RD Internal Shock via Confinement Fermi limit IS Synchro. Photosphere Original Paczynski Goodman G* ~103 Photon-to-Baryon h*~103 h=E/Mc2

  23. Implications • Lorentz factor: Cutoff probed by CTA • Non-thermal spectrum ~ Band • Extended g generation, deep inside g-sphere • Early afterglow, High efficiency is possible • GeV lag ~ rphotosphere/cGfc2 • UHECR, neutrino • Magnetic field dissipation • Blandford-Znajek McKinney

  24. B Amplification & Decay behind shock f=1.8 T. Inoue, Asano & KI 11

  25. Most Ancient Object GRB 090423 @ z~8.2 A massive star’s death just 600 Myr after the Big Bang

  26. First GRB Abel+ 02 Bromm+ 02 Omukai+ 03 Yoshida+ 08 Pop III (Zero Metal) ~100-1000M(!?) Present Day Massive Star ~20M Komissarov & Barkov 10 Meszaros & Rees 10 Gigantic (x100) GRB @ z~10-30???

  27. Massive Envelope R/c~103s > TGRB~10s ⇒ No GRB? No mass loss via line driven wind Envelope Core Ohkubo+ 09 Heger+ 03 Suwa & KI 10

  28. Envelope Accretion ⇒ vJet head • Energetic • Very long • Modest L • Bright phase • ⇒ Cocoon Suwa & KI 10

  29. Analytic Expressions

  30. GRB jet can breakout the first star!

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