Very High Lorentz Factor Fireballs and Gamma-Ray Burst Spectra

被引:45
作者
Ioka, Kunihito [1 ,2 ]
机构
[1] KEK Theory Ctr, Tsukuba, Ibaraki 3050801, Japan
[2] Grad Univ Adv Studies Sokendai, Tsukuba, Ibaraki 3050801, Japan
来源
PROGRESS OF THEORETICAL PHYSICS | 2010年 / 124卷 / 04期
关键词
HIGH-ENERGY EMISSION; RELATIVISTIC COLLISIONLESS SHOCKS; PROMPT EMISSION; FERMI OBSERVATIONS; AFTERGLOW EMISSION; INTERNAL SHOCKS; MAGNETIC-FIELDS; PHOTOSPHERIC EMISSION; PHYSICAL PARAMETERS; THERMAL EMISSION;
D O I
10.1143/PTP.124.667
中图分类号
O4 [物理学];
学科分类号
0702 ;
摘要
Collision less entrainment of the surrounding matter imports the relativistic baryon component in the Gamma-Ray Burst (GRB) fireball frame. We show that half the fireball energy can be transferred from radiation to the comoving hot motions of baryons under the photosphere. The yet baryon-poor fireball can reexpand to a very high Lorentz factor (VHLF) Gamma similar to 10(3)-10(6) by its own relativistic collisionless pressure beyond the photosphere (so-called collisionless bulk acceleration), leading to internal and external shocks. A simple synchrotron emission from the VHLF internal shocks produces (i) the extra power-law spectral component with variability observed in the Fermi GeV bursts, up to the TeV range for the future Cherenkov Telescope Array (CTA), (ii) the GeV onset delay with a weak luminosity dependence t(delay) similar to L-1/5, and (iii) the spectral break of GRB 090926 by the synchrotron cooling break or the maximum synchrotron cutoff limited by the dynamical time, not by the e creation cutoff. The relativistic baryon component could also heat the photospheric thermal photons into the main GRB Band spectrum via pp, p gamma (Bethe-Heitler and photomeson), and Coulomb thermalization processes. In this hot photosphere-internal-external shock model, we can predict the anticorrelation of similar to TeV neutrinos and GeV gamma-rays, which may be detectable using Ice Cube. The spectral peak and luminosity (Yonetoku) relation is also reproduced if the progenitor stars are nearly identical. We also discuss the steep/shallow decay of early X-ray afterglows and short GRBs.
引用
收藏
页码:667 / 710
页数:44
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