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Ultra Long Gamma-Ray Bursts from the collapse of Blue Super Giant stars: an end-to-end simulation

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arxiv 1803.04983 v2 pith:QJUULVZR submitted 2018-03-13 astro-ph.HE

Rosalba Perna , Davide Lazzati , Matteo Cantiello This is my paper · ORCID
classification astro-ph.HE
keywords accretionlongsimulationbluebsgsburstscodecollapse
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

Ultra-long gamma ray bursts (ULGRBs) are a distinct class of GRBs characterized by durations of several thousands of seconds, about two orders of magnitude longer than those of standard long GRBs (LGRBs). The driving engine of these events has not been uncovered yet, and ideas range from magnetars, to tidal disruption events, to extended massive stars, such as blue super giants (BSG). BSGs, a possible endpoint of stellar evolution, are attractive for the relatively long free-fall times of their envelopes, allowing accretion to power a long-lasting central engine. At the same time, their large radial extension poses a challenge to the emergence of a jet. Here we perform an end-to-end simulation aimed at assessing the viability of BSGs as ULGRB progenitors. The evolution to core collapse of a BSG star model is calculated with the MESA code. We then compute the accretion rate for the fraction of envelope material with enough angular momentum to circularize and form an accretion disk, and input the corresponding power into a jet which we evolve through the star envelope with the FLASH code. Our simulation shows that the jet can emerge, and the resulting light curves resemble those observed in ULGRBs, with durations $T_{90}$ ranging from $\approx$4000~s to $\approx10^4$ s depending on the viewing angle.

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Forward citations

Cited by 5 Pith papers

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  2. Formation of rotating supergiants via stellar mergers in dense clusters: Implications for black hole natal spins

    astro-ph.HE 2026-07 conditional novelty 6.0 of 10

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    astro-ph.HE 2025-01 unverdicted novelty 1.0 of 10

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