On the Induced Gravitational Collapse: SPH Simulations
- Autores: Becerra L.1,2, Ellinger C.3, Fryer C.3, Rueda J.A.1,2,4, Ruffini R.1,2,4
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Afiliações:
- ICRA and University of Rome “Sapienza,”
- ICRANet
- CCS-2
- ICRANet-Rio
- Edição: Volume 62, Nº 12 (2018)
- Páginas: 840-846
- Seção: Article
- URL: https://journals.rcsi.science/1063-7729/article/view/191951
- DOI: https://doi.org/10.1134/S1063772918120168
- ID: 191951
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Resumo
The Induced Gravitational Collapse (IGC) paradigm points to a binary origin for the longduration gamma-ray burst (GRBs) associated with supernovae (SN). In this one, a carbon-oxygen core (COcore) explodes in a Type Ib/c SN in presence of a close neutron star (NS) companion. The SN triggers a hypercritical accretion into the NS and depending on the initial binary parameters, two outcomes are possible givimg place to two family of long GRBs: binary-driven hypernova (BdHNe), where the NS reaches its critical mass, and collapses to a black hole (BH), emitting a GRB; and x-ray flashes (XRFs) where the hypercritical accretion onto the NS is not sufficient to induce its gravitational collapse. We perform 3-dimensional (3D) numerical simulations of the IGC paradigm with the smoothed particle hydrodynamics (SPH) technique. We determine whether the star gravitational collapse is possible and assess if the binary holds gravitationally bound or it becomes unbound by the SN explosion.
Sobre autores
L. Becerra
ICRA and University of Rome “Sapienza,”; ICRANet
Autor responsável pela correspondência
Email: Laura.Becerra@icranet.org
Itália, Rome; Pescara
C. Ellinger
CCS-2
Email: Laura.Becerra@icranet.org
Estados Unidos da América, Los Alamos
C. Fryer
CCS-2
Email: Laura.Becerra@icranet.org
Estados Unidos da América, Los Alamos
J. Rueda
ICRA and University of Rome “Sapienza,”; ICRANet; ICRANet-Rio
Email: Laura.Becerra@icranet.org
Itália, Rome; Pescara; Rio de Janeiro
R. Ruffini
ICRA and University of Rome “Sapienza,”; ICRANet; ICRANet-Rio
Email: Laura.Becerra@icranet.org
Itália, Rome; Pescara; Rio de Janeiro
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