Primordial black hole origin for thermal gamma-ray bursts. (arXiv:2007.11226v3 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Barco_O/0/1/0/all/0/1">Oscar del Barco</a>
A binary black hole (BH) astrophysical scenario where a mass-constrained
($2.5 times 10^{-13} M_{sun}$) primordial black hole (PBH) undergoes a radial
fall onto its heavier component (such as a supermassive black hole (SMBH)) is
described as an intense gamma-ray emission event. As the relativistic PBH
approaches the Schwarschild SMBH event horizon, its Lorentz-boosted Hawking
radiation progressively reduces to a near-zero emission cone resulting in a
highly collimated thermal beam. Accordingly, our numerically calculated PBH
flux density $S_{nu}$ and $nu S_{nu}$ fluence spectrum show a decreasing
Planck-like spectral dependence consistent with the cooling behaviour of
thermal-dominant gamma-ray bursts (GRBs). Our results might provide an
alternative explanation for thermal GRBs based on PBH origin.
A binary black hole (BH) astrophysical scenario where a mass-constrained
($2.5 times 10^{-13} M_{sun}$) primordial black hole (PBH) undergoes a radial
fall onto its heavier component (such as a supermassive black hole (SMBH)) is
described as an intense gamma-ray emission event. As the relativistic PBH
approaches the Schwarschild SMBH event horizon, its Lorentz-boosted Hawking
radiation progressively reduces to a near-zero emission cone resulting in a
highly collimated thermal beam. Accordingly, our numerically calculated PBH
flux density $S_{nu}$ and $nu S_{nu}$ fluence spectrum show a decreasing
Planck-like spectral dependence consistent with the cooling behaviour of
thermal-dominant gamma-ray bursts (GRBs). Our results might provide an
alternative explanation for thermal GRBs based on PBH origin.
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