On the Ultra-relativistic Prompt Emission, the Hard and Soft X-Ray Flares, and the Extended Thermal Emission in GRB 151027A

• Published in: The Astrophysical journal Vol. 869; no. 2; pp. 151 - 165
• Main Authors: Ruffini, R., Becerra, L., Bianco, C. L., Chen, Y. C., Karlica, M., Kova evi, M., Fuksman, J. D. Melon, Moradi, R., Muccino, M., Pisani, G. B., Primorac, D., Rueda, J. A., Vereshchagin, G. V., Wang, Y., Xue, S. S.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 20-12-2018; IOP Publishing
• Subjects: Astrophysics; binaries: general; Binary stars; black hole physics; Black holes; Companion stars; Computational fluid dynamics; Computer simulation; Deposition; Ejecta; Emission analysis; Emissions; Flares; Fluid flow; Gamma ray bursts; Gamma rays; gamma-ray burst: general; Gravitational collapse; Hydrodynamics; Morphology; Neutron stars; Oxygen; Relativism; Relativistic effects; Smooth particle hydrodynamics; Soft x rays; stars: neutron; Supernova; supernovae: general; Thermal emission
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aaee68

We analyze GRB 151027A within the binary-driven hypernova approach, with a progenitor of a carbon-oxygen core on the verge of a supernova (SN) explosion and a binary companion neutron star (NS). The hypercritical accretion of the SN ejecta onto the NS leads to its gravitational collapse into a black hole (BH), to the emission of the gamma-ray burst (GRB), and to a copious e+e− plasma. The impact of this e+e− plasma on the SN ejecta explains the early soft X-ray flare observed in long GRBs. Here, we apply this approach to the ultra-relativistic prompt emission (UPE) and to the hard X-ray flares. We use GRB 151027A as a prototype. From the time-integrated and the time-resolved analysis, we identify a double component in the UPE and confirm its ultra-relativistic nature. We confirm the mildly relativistic nature of the soft X-ray flare, of the hard X-ray flare, and of the extended thermal emission (ETE). We show that the ETE identifies the transition from an SN to a hypernova (HN). We then address the theoretical justification of these observations by integrating the hydrodynamical propagation equations of the e+e− into the SN ejecta, with the latter independently obtained from 3D smoothed particle hydrodynamics simulations. We conclude that the UPE, the hard X-ray flare, and the soft X-ray flare do not form a causally connected sequence. Within our model, they are the manifestation of the same physical process of the BH formation as seen through different viewing angles, implied by the morphology and the ∼300 s rotation period of the HN ejecta.