On the GeV emission of the type I BdHN GRB 130427A

Remo Ruffini (Author), Rahim Moradi (Author), J. A. Rueda (Author), L. Becerra (Author), C. L. Bianco (Author), C. Cherubini (Author), S. Filippi (Author), Y. C. Chen (Author), Mile Karlica (Author), N. Sahakyan (Author), Y. Wang (Author), S. S. Xue (Author)

Abstract

We propose that the inner engine of a type I binary-driven hypernova (BdHN) is composed of Kerr black hole (BH) in a non-stationary state, embedded in a uniform magnetic field B_0 aligned with the BH rotation axis and surrounded by an ionized plasma of extremely low density of 10^−14 g cm−3. Using GRB 130427A as a prototype, we show that this inner engine acts in a sequence of elementary impulses. Electrons accelerate to ultrarelativistic energy near the BH horizon, propagating along the polar axis, θ = 0, where they can reach energies of ~10^18 eV, partially contributing to ultrahigh-energy cosmic rays. When propagating with $\theta \ne 0$ through the magnetic field B_0, they produce GeV and TeV radiation through synchroton emission. The mass of BH, M = 2.31M ⊙, its spin, α = 0.47, and the value of magnetic field B_0 = 3.48 × 10^10 G, are determined self consistently to fulfill the energetic and the transparency requirement. The repetition time of each elementary impulse of energy ${ \mathcal E }\sim {10}^{37}$ erg is ~10^−14 s at the beginning of the process, then slowly increases with time evolution. In principle, this "inner engine" can operate in a gamma-ray burst (GRB) for thousands of years. By scaling the BH mass and the magnetic field, the same inner engine can describe active galactic nuclei.

Keywords

black hole physics;binaries;gamma-ray burst;neutron;stars;supernovae;

Data

Language:	English
Year of publishing:	2019
Typology:	1.01 - Original Scientific Article
Organization:	UNG - University of Nova Gorica
UDC:	52
COBISS:	23009283
ISSN:	1538-4357
Views:	2091
Downloads:	0
Average score:	0 (0 votes)
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Other data

URN:	URN:SI:UNG
Type (COBISS):	Not categorized
Pages:	str. 1-13
Volume:	ǂVol. ǂ886
Issue:	ǂno. ǂ2
Chronology:	Nov. 2019
DOI:	10.3847/1538-4357/ab4ce6
ID:	11908594