Long Duration X-Ray Flash and X-Ray Rich Gamma Ray Burst from Low Mass Population III Star

Abstract

Recent numerical simulations suggest that Population III (Pop III) stars were born with masses not larger than $\sim 100M_{\odot }$ but typically $\sim 40M_{\odot }$. By self-consistently considering the jet generation and propagation in the envelope of these low mass Pop III stars, we find that a Pop III blue super giant star has the possibility to raise a gamma-ray burst (GRB) even though it keeps a massive hydrogen envelope. We evaluate observational characters of Pop III GRBs and predict that Pop III GRBs have the duration of $\sim 10^5$ sec in the observer frame and the peak luminosity of $\sim 5\times 10^{50}\mathrm{erg}{\sec }^{-1}$. Assuming that the $E_p-L_p$ (or $E_p-E_{\gamma ,\mathrm{iso}}$) correlation holds for Pop III GRBs, we find that the spectrum peak energy falls $\sim$ a few keV (or $\sim 100$ keV) in the observer frame. We discuss the detectability of Pop III GRBs by future satellite missions such as EXIST and Lobster. If the $E_p-E_{\gamma ,\mathrm{iso}}$ correlation holds, we have the possibility to detect Pop III GRBs at $z\sim 9$ as long duration X-ray rich GRBs by EXIST. On the other hand, if the $E_p-L_p$ correlation holds, we have the possibility to detect Pop III GRBs up to $z\sim 19$ as long duration X-ray flashes by Lobster.

27 pages, 7 figures, Accepted to the Astrophysical Journal

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