Constraints on Gamma-ray Burst Inner Engines in a Blandford-Znajek Framework. (arXiv:1902.01974v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lloyd_Ronning_N/0/1/0/all/0/1">Nicole M. Lloyd-Ronning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fryer_C/0/1/0/all/0/1">Chris Fryer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_J/0/1/0/all/0/1">Jonah Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prasad_N/0/1/0/all/0/1">Neelima Prasad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Torres_C/0/1/0/all/0/1">Chris Torres</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_P/0/1/0/all/0/1">Phillip Martin</a>
Under the assumption that a Gamma-ray Burst (GRB) is ultimately produced by a
Blandford-Znajek (BZ) jet from a highly spinning black hole BH, we put limits
on the magnetic field and BH mass needed to power observed long and short GRBs.
For BHs in the range of $2-10 M_{odot}$ (for long GRBs) and $0.5-4 M_{odot}$
(for short GRBs), we find magnetic fields in the range of $5×10^{14} lesssim B
lesssim 10^{17}$ G are needed to power the observed GRBs. Under the simple
assumption of flux conservation, we estimate the magnetic fields of the
progenitor systems for both long and short GRBs, finding that single massive
star progenitors require fields $sim 10^{6}$ G and NS merger systems require
fields $sim 10^{15}$ G. We also discuss the implications and consequences of
high magnetic fields in GRB BH-disk systems, in terms of MRI field growth and
magnetically arrested disks. Finally, we examine the conditions under which the
progenitor systems can retain enough angular momentum to create BHs spinning
rapidly enough to power BZ jets.
Under the assumption that a Gamma-ray Burst (GRB) is ultimately produced by a
Blandford-Znajek (BZ) jet from a highly spinning black hole BH, we put limits
on the magnetic field and BH mass needed to power observed long and short GRBs.
For BHs in the range of $2-10 M_{odot}$ (for long GRBs) and $0.5-4 M_{odot}$
(for short GRBs), we find magnetic fields in the range of $5×10^{14} lesssim B
lesssim 10^{17}$ G are needed to power the observed GRBs. Under the simple
assumption of flux conservation, we estimate the magnetic fields of the
progenitor systems for both long and short GRBs, finding that single massive
star progenitors require fields $sim 10^{6}$ G and NS merger systems require
fields $sim 10^{15}$ G. We also discuss the implications and consequences of
high magnetic fields in GRB BH-disk systems, in terms of MRI field growth and
magnetically arrested disks. Finally, we examine the conditions under which the
progenitor systems can retain enough angular momentum to create BHs spinning
rapidly enough to power BZ jets.
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