Angular Momentum Role in the Hypercritical Accretion of Binary-Driven Hypernovae

Becerra, L.; Cipolletta, Federico; Fryer, Chris L.; Rueda, J. A.; Ruffini, Remo

doi:10.1088/0004-637x/812/2/100

Cited by 59 publications

(176 citation statements)

References 32 publications

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“…In the case of long GRBs we stand on the induced gravitational collapse (IGC) scenario that introduces as their progenitors short-period binaries composed of a carbon-oxygen core (CO core ) with a NS companion [9][10][11][12][13][14][15]. The core-collapse of the CO core , which forms a NS as central remnant (hereafter νNS), leads also to a SN explosion that triggers a massive, hypercritical accretion process onto the NS companion.…”

Section: Long Grbsmentioning

confidence: 99%

“…Long bursts with E iso 10 52 erg are instead produced by more compact CO core -NS binaries (a 10 11 cm, see e.g., Refs. [13,15]). In this case the SN triggers a larger accretion rate onto the NS companion, e.g.…”

Section: Long Grbsmentioning

confidence: 99%

“…[12] and [13]), Eq. (1) gives accretion rates around the order of 10 −4 − 10 −2 M s −1 , and an angular momentum per unit time crossing the capture regionL cap ∼ 10 46 -10 49 g cm 2 s −2 .…”

Section: Igc Hypercritical Accretion and Long Grbsmentioning

confidence: 99%

“…It was shown in Ref. [13] the existence of a maximum orbital period, P max , over which the accretion onto NS companion is not high enough to bring it to the critical mass for gravitational collapse to a BH. Therefore, CO core -NS binaries with P > P max lead to XRFs while the ones with P P max lead to BdHNe.…”

Section: Most Recent Simulations Of the Igc Processmentioning

confidence: 99%

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The binary progenitors of short and long GRBs and their gravitational-wave emission

et al. 2018

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Abstract. We have sub-classified short and long-duration gamma-ray bursts (GRBs) into seven families according to the binary nature of their progenitors. Short GRBs are produced in mergers of neutron-star binaries (NS-NS) or neutron star-black hole binaries (NS-BH). Long GRBs are produced via the induced gravitational collapse (IGC) scenario occurring in a tight binary system composed of a carbon-oxygen core (CO core ) and a NS companion. The CO core explodes as type Ic supernova (SN) leading to a hypercritical accretion process onto the NS: if the accretion is sufficiently high the NS reaches the critical mass and collapses forming a BH, otherwise a massive NS is formed. Therefore long GRBs can lead either to NS-BH or to NS-NS binaries depending on the entity of the accretion. We discuss for the above compact-object binaries: 1) the role of the NS structure and the nuclear equation of state; 2) the occurrence rates obtained from X and gamma-rays observations; 3) the predicted annual number of detections by the Advanced LIGO interferometer of their gravitational-wave emission.

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Section: Long Grbsmentioning

confidence: 99%

Section: Long Grbsmentioning

confidence: 99%

Section: Igc Hypercritical Accretion and Long Grbsmentioning

confidence: 99%

Section: Most Recent Simulations Of the Igc Processmentioning

confidence: 99%

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The binary progenitors of short and long GRBs and their gravitational-wave emission

et al. 2018

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“…However, the above single progenitor model contrasts with -X-ray flashes (XRFs) with E iso 10 52 erg and restframe spectral peak energy E p,i 200 keV. These systems, already pioneered in a different context [43][44][45], originate in widely separated CO core -NS binaries with an orbital separation a > 10 11 cm [41], therefore the hypercritical accretion onto the NS companion is insufficient to induce gravitational collapse to a BH [39][40][41] and, therefore, as expected in our theory no GeV emission is observed. The outcomes (or out-states) of XRFs are binaries composed of a new NS (νNS) produced from the SN explosion, and a massive NS (MNS) which accreted matter from the SN ejecta.…”

Section: Introductionmentioning

confidence: 99%

What can we learn from GRBs?

et al. 2018

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Abstract. We review our recent results on the classification of long and short gamma-ray bursts (GRBs) in different subclasses. We provide observational evidences for the binary nature of GRB progenitors. For long bursts the induced gravitational collapse (IGC) paradigm proposes as progenitor a tight binary system composed of a carbon-oxygen core (CO core ) and a neutron star (NS) companion; the supernova (SN) explosion of the CO core triggers a hypercritical accretion process onto the companion NS. For short bursts a NS-NS merger is traditionally adopted as the progenitor. We also indicate additional sub-classes originating from different progenitors: (CO core )-black hole (BH), BH-NS, and white dwarf-NS binaries. We also show how the outcomes of the further evolution of some of these sub-classes may become the progenitor systems of other sub-classes.

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Some recent results on neutrino osillations in hypercritical accretion

Uribe-Suárez

Rueda

2019

Astron Nachr

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The study of neutrino flavor oscillations in astrophysical sources has been boosted in the last two decades thanks to achievements in experimental neutrino physics and in observational astronomy. We here discuss two cases of interest in the modeling of short and long gamma-ray bursts: hypercritical, that is, highly super-Eddington spherical/disk accretion onto a neutron star/black hole.We show that in both systems, the ambient conditions of density and temperature imply the occurrence of neutrino flavor oscillations, with a relevant role of neutrino self-interactions. K E Y W O R D Sblack hole, gamma-ray bursts, neutrino flavor oscillations, neutron star 1 Astron. Nachr. / AN. 2019;340:935-944.www.an-journal.org

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Angular Momentum Role in the Hypercritical Accretion of Binary-Driven Hypernovae

Cited by 59 publications

References 32 publications

The binary progenitors of short and long GRBs and their gravitational-wave emission

The binary progenitors of short and long GRBs and their gravitational-wave emission

What can we learn from GRBs?

Some recent results on neutrino osillations in hypercritical accretion

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