Signatures of neutrino cooling in the SN1987A scenario

Fraija, N.; Bernal, C. G.; Hidalgo-Gámez, A. M.

doi:10.1093/mnras/stu872

Cited by 17 publications

(16 citation statements)

References 42 publications

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“…Moreover, Chevalier (1989) estimated a total fallback around 0.1 M ⊙ for SN 1987A, which is supposed to be an unusually high value compared to "normal" type II supernovae. Recent multi-dimensional numerical simulations by Bernal et al (2013); Fraija et al (2014) confirmed this scenario and furthermore showed that such a hypercritical accretion can lead to a submergence of the magnetic field, giving a natural explanation why the neutron star (possibly) born in SN 1987A has not been found yet.…”

Section: Amount Of Fallbackmentioning

confidence: 89%

Pushing Core-Collapse Supernovae to Explosions in Spherical Symmetry. I. The Model and the Case of Sn 1987a

Perego

Hempel

Fröhlich

et al. 2015

ApJ

116

153

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We report on a method, PUSH, for artificially triggering core-collapse supernova explosions of massive stars in spherical symmetry. We explore basic explosion properties and calibrate PUSH to reproduce SN 1987A observables. Our simulations are based on the GR hydrodynamics code AGILE combined with the neutrino transport scheme IDSA for electron neutrinos and ASL for the heavy flavor neutrinos. To trigger explosions in the otherwise non-exploding simulations, the PUSH method increases the energy deposition in the gain region proportionally to the heavy flavor neutrino fluxes. We explore the progenitor range 18 -21 M ⊙ . Our studies reveal a distinction between high compactness (HC) (compactness parameter ξ 1.75 > 0.45) and low compactness (LC) (ξ 1.75 < 0.45) progenitor models, where LC models tend to explode earlier, with a lower explosion energy, and with a lower remnant mass. HC models are needed to obtain explosion energies around 1 Bethe, as observed for SN 1987A. However, all the models with sufficiently high explosion energy overproduce 56 Ni and fallback is needed to reproduce the observed nucleosynthesis yields. 57−58 Ni yields depend sensitively on the electron fraction and on the location of the mass cut with respect to the shell structure of the progenitor. We identify a progenitor and a suitable set of parameters that fit the explosion properties of SN 1987A assuming 0.1 M ⊙ of fallback. We predict a neutron star with a gravitational mass of 1.50 M ⊙ . We find correlations between explosion properties and the compactness of the progenitor model in the explored mass range. However, a more complete analysis will require exploring of a larger set of progenitors.

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Section: Amount Of Fallbackmentioning

confidence: 89%

Pushing Core-Collapse Supernovae to Explosions in Spherical Symmetry. I. The Model and the Case of Sn 1987a

Perego

Hempel

Fröhlich

et al. 2015

ApJ

116

153

View full text Add to dashboard Cite

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“…This resonance depends on the effective potential and neutrino oscillation parameters. The equations that determine the neutrino evolution in matter for two and three flavors are related as follows [27,56].…”

Section: Iii12 Resonant Oscillationsmentioning

confidence: 99%

Could a plasma in quasi-thermal equilibrium be associated to the “orphan” TeV flares?

Fraija

2015

Astroparticle Physics

Self Cite

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a b s t r a c tTeV γ -ray detections in flaring states without activity in X-rays from blazars have attracted much attention due to the irregularity of these "orphan" flares. Although the synchrotron self-Compton model has been very successful in explaining the spectral energy distribution and spectral variability of these sources, it has not been able to describe these atypical flaring events. On the other hand, an electron-positron pair plasma at the base of the AGN jet was proposed as the mechanism of bulk acceleration of relativistic outflows. This plasma in quasi-thermal equilibrium called Wein fireball emits radiation at MeV-peak energies serving as target of accelerated protons. In this work we describe the "orphan" TeV flares presented in blazars 1ES 1959+650 and Mrk 421 assuming geometrical considerations in the jet and evoking the interactions of Fermi-accelerated protons and MeV-peak target photons coming from the Wein fireball. After describing successfully these "orphan" TeV flares, we correlate the TeV γ -ray, neutrino and UHECR fluxes through pγ interactions and calculate the number of high-energy neutrinos and UHECRs expected in IceCube/AMANDA and TA experiment, respectively. In addition, thermal MeV neutrinos produced mainly through electron-positron annihilation at the Wein fireball will be able to propagate through it. By considering two-(solar, atmospheric and accelerator parameters) and three-neutrino mixing, we study the resonant oscillations and estimate the neutrino flavor ratios as well as the number of thermal neutrinos expected on Earth.

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“…Under normal SN conditions, over 99% of the energy released leaves the star as neutrinos, without further interaction. For SN 1987A [13] the kinetic energy was around E kin ∼ 1 B and the total energy released (in neutrinos) was E T ∼ 300 B. Assuming somewhat larger efficiency (larger density and temperature, thus, larger neutrino cross section), and considering we have more mass in the compact object we estimate the kinetic energy to be a few times larger than in SN 1987A, i.e., E kin ∼ 5 B, which coincides with the observations for GRB 110709B.…”

Section: Act Ii: Bh Formationmentioning

confidence: 99%

Three-peak GRBs and their implications for central engines

2015

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GRB 110709B presented a peculiar three-peak lightcurve; this burst twice triggered the BAT detector onboard Swift. The two triggers were separated by ∼ 10 minutes. In order to explain such an event, we unify into a single description the millisecond (ms) protomagnetar and the collapsar central-engine models. We find that such a scenario could produce GRBs with three peaks. One for the ms-protomagnetar stage, a second one for the BH-formation event and a third one for the collapsar phase. We show that the three peaks for GRB 110709B originate from different phases of the same collapsing object. We estimate the energies and timescales of the different episodes of this burst using our model and compare with previous results as well as with a reanalysis we perform on the data. We show that not only the light curve, but also the photon index evolution and the delay between the prompt emission and the afterglow of the second central-engine activity phase point towards a model like the one proposed here. We find that, with reasonable assumptions, our model correctly describes the activity in GRB 110709B. We further suggest careful study of future GRBs lightcurves which may help show the validity of our model. If our model is correct, this would be the first time that the formation of a BH from a core-collapse event is observed unimpededly.

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Signatures of neutrino cooling in the SN1987A scenario

Cited by 17 publications

References 42 publications

Pushing Core-Collapse Supernovae to Explosions in Spherical Symmetry. I. The Model and the Case of Sn 1987a

Pushing Core-Collapse Supernovae to Explosions in Spherical Symmetry. I. The Model and the Case of Sn 1987a

Could a plasma in quasi-thermal equilibrium be associated to the “orphan” TeV flares?

Three-peak GRBs and their implications for central engines

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