1 / 31

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.

harper
Télécharger la présentation

Gamma-Ray Bursts from Radiation-Dominated Jet?

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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!

More Related