Neutrino Oscillations within the Induced Gravitational Collapse Paradigm of Long Gamma-Ray Bursts

Becerra, L.; Guzzo, M. M.; Rossi-Torres, F.; Rueda, J. A.; Ruffini, Remo; Uribe, Juan D.

doi:10.3847/1538-4357/aaa296

Cited by 33 publications

(48 citation statements)

References 86 publications

(136 reference statements)

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…The neutrino luminosity can reach values of up to 10 52 erg s −1 and the neutrino mean energy of 20 MeV for the above upper value of the accretion rate. For the reader interested in the neutrino emission, we refer to [93] for a detailed analysis of the neutrino production in XRFs and BdHNe including flavor oscillations experienced by the neutrinos before abandoning the system.…”

Section: First 3d Simulationsmentioning

confidence: 99%

See 1 more Smart Citation

Induced Gravitational Collapse, Binary-Driven Hypernovae, Long Gramma-ray Bursts and Their Connection with Short Gamma-ray Bursts

2019

Self Cite

View full text Add to dashboard Cite

There is increasing observational evidence that short and long Gamma-ray bursts (GRBs) originate in different subclasses, each one with specific energy release, spectra, duration, etc, and all of them with binary progenitors. The binary components involve carbon-oxygen cores (CO core ), neutron stars (NSs), black holes (BHs), and white dwarfs (WDs). We review here the salient features of the specific class of binary-driven hypernovae (BdHNe) within the induced gravitational collapse (IGC) scenario for the explanation of the long GRBs. The progenitor is a CO core -NS binary. The supernova (SN) explosion of the CO core , producing at its center a new NS (νNS), triggers onto the NS companion a hypercritical, i.e., highly super-Eddington accretion process, accompanied by a copious emission of neutrinos. By accretion the NS can become either a more massive NS or reach the critical mass for gravitational collapse with consequent formation of a BH. We summarize the results on this topic from the first analytic estimates in 2012 all the way up to the most recent three-dimensional (3D) smoothed-particle-hydrodynamics (SPH) numerical simulations in 2018. Thanks to these results it is by now clear that long GRBs are richer and more complex systems than thought before. The SN explosion and its hypercritical accretion onto the NS explain the X-ray precursor. The feedback of the NS accretion, the NS collapse and the BH formation produce asymmetries in the SN ejecta, implying the necessity of a 3D analysis for GRBs. The newborn BH, the surrounding matter and the magnetic field inherited from the NS, comprises the inner engine from which the GRB electron-positron (e + e − ) plasma and the high-energy emission are initiated. The impact of the e + e − on the asymmetric ejecta transforms the SN into a hypernova (HN). The dynamics of the plasma in the asymmetric ejecta leads to signatures depending on the viewing angle. This explains the ultrarelativistic prompt emission in the MeV domain and the mildly-relativistic flares in the early afterglow in the X-ray domain. The feedback of the νNS pulsar-like emission on the HN explains the X-ray late afterglow and its power-law regime. All of the above is in contrast with a simple GRB model attempting to explain the entire GRB with the kinetic energy of an ultrarelativistic jet extending through all of the above GRB phases, as traditionally proposed in the "collapsar-fireball" model. In addition, BdHNe in their different flavors lead to νNS-NS or νNS-BH binaries. The gravitational wave emission drives these binaries to merge producing short GRBs. It is thus established a previously unthought interconnection between long and short GRBs and their occurrence rates. This needs to be accounted for in the cosmological evolution of binaries within population synthesis models for the formation of compact-object binaries.

show abstract

Section: First 3d Simulationsmentioning

confidence: 99%

“…The accretion power can be as high as L acc ∼ 0.1Ṁ b c 2 ∼ 10 47 -10 51 erg s −1 for accretion rates in the rangė M b ∼ 10 −6 -10 −2 M s −1 . Figure 4 in [93]). The electron-neutrino survival probability is shown as a function of the radial distance from the NS surface.…”

Section: Accretion Luminositymentioning

confidence: 99%

Induced Gravitational Collapse, Binary-Driven Hypernovae, Long Gramma-ray Bursts and Their Connection with Short Gamma-ray Bursts

2019

Self Cite

View full text Add to dashboard Cite

show abstract

“…The neutrino emissivity can be approximated with a very good accuracy by (Yakovlev et al ).

\begin{array}{l} ϵ_{i}^{m} \approx \frac{2 G_{F}^{2} {(T)}^{8 + m}}{9 π^{5}} C_{+, i}^{2} false[ℱ_{m + 1, 0} ((), η_{e^{+}}) ℱ_{1, 0} ((), η_{e^{-}}) \\ + ℱ_{m + 1, 0} ((), η_{e^{-}}) ℱ_{1, 0} ((), η_{e^{+}}) false], \end{array}

where ℱ k , ℓ ( y , η ) are the generalized Fermi functions (see [Becerra et al ] for details) and ℱ k , ℓ ( η ) = ℱ k , ℓ ( y = 0, η ). For m = 0 and m = 1 Equation (12) gives the neutrino and antineutrino number emissivity (neutrino production rate), and the neutrino and antineutrino energy emissivity (energy per unit volume per unit time) for a certain flavor i , respectively.…”

Section: Neutrino Oscillationsmentioning

confidence: 99%

“…Finally, we note that for accretion rates

\dot{M} < 5 \times 10^{- 5} M_{⊙}

s −1 , either the matter potential is close enough to the vacuum potential and the MSW condition is satisfied, or both the self‐interaction and matter potentials are so low that the flavor oscillations are only due to the vacuum potential. In both cases, bipolar oscillations are not present (Becerra et al ). Without bipolar oscillations, it is not possible to guarantee that decoherence will be complete and Equation (20) is no longer valid.…”

Section: Neutrino Oscillationsmentioning

confidence: 99%

Some recent results on neutrino osillations in hypercritical accretion

Uribe-Suárez

Rueda

2019

Astron Nachr

View full text Add to dashboard Cite

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

show abstract

“…Gravitational waves are produced (Oliveira et al 2014) together with GeV emission from the accretion onto the Kerr BH (Ruffini et al 2018). It has been shown (Becerra et al 2018) that the accretion onto the NS generates neutrino-antineutrino emission in the case of long GRBs, and this emission has been explained as due to e − e +pair annihilation.…”

Section: Introductionmentioning

confidence: 99%

Neutrino Oscillations and Decoherence in Short-GRB Progenitors

Penacchioni

Civitarese

2019

ApJ

View full text Add to dashboard Cite

Neutrinos are produced in cosmic accelerators, like active galactic nuclei (AGNs), blazars, supernova (SN) remnants and gamma-ray bursts (GRBs). On their way to the Earth they experience flavor-oscillations. The interactions of the neutrinos coming from the source with other particles, e.g. intergalactic primordial neutrinos or heavy-mass right-handed neutrinos, in their way to the detector may transform the original wave packet in pointer states. This phenomenon, known as decoherence, becomes important in the reconstruction of processes at the source. In this work we study neutrino emission in short GRBs by adopting the Fireshell Model. We consider e − e + -pair annihilation as the main channel for neutrino production. We compare the properties of the neutrino-flux with the characteristic photon-signal produced once the transparency condition is reached. We study the effects of flavor-oscillations and decoherence as neutrinos travel from the region near the blackhole (BH) event-horizon outwards. We consider the source to be in thermal equilibrium, and calculate energy distribution functions for electrons and neutrinos. To compute the effects of decoherence we use a Gaussian model. In this scenario the emitted electron-neutrinos transform into pointer states consisting of 67.8% electronneutrinos and 32.2% as a combination of mu and tau neutrinos. We found that decoherence plays an important role in the evolution of the neutrino wave packet, leading to the detected pointer states on Earth.

show abstract

Neutrino Oscillations within the Induced Gravitational Collapse Paradigm of Long Gamma-Ray Bursts

Cited by 33 publications

References 86 publications

Induced Gravitational Collapse, Binary-Driven Hypernovae, Long Gramma-ray Bursts and Their Connection with Short Gamma-ray Bursts

Induced Gravitational Collapse, Binary-Driven Hypernovae, Long Gramma-ray Bursts and Their Connection with Short Gamma-ray Bursts

Some recent results on neutrino osillations in hypercritical accretion

Neutrino Oscillations and Decoherence in Short-GRB Progenitors

Contact Info

Product

Resources

About