scholarly journals Analytic solutions for neutrino-light curves of core-collapse supernovae

2020 ◽  
Author(s):  
Yudai Suwa ◽  
Akira Harada ◽  
Ken’ichiro Nakazato ◽  
Kohsuke Sumiyoshi
Keyword(s):  
Radiation Transport ◽  
Numerical Models ◽  
Average Energy ◽  
Analytic Solutions ◽  
Core Collapse ◽  
Central Engine ◽  
Supernova Explosions ◽  
Protoneutron Stars ◽  
Neutrino Luminosity ◽  
Physical Quantities

Abstract Neutrino is a guaranteed signal from supernova explosions in the Milky Way and is the most valuable messenger that can provide us with information about the deepest part of supernovae. In particular, neutrinos will provide us with physical quantities, such as the radius and mass of protoneutron stars (PNS), which are the central engine of supernovae. It requires a theoretical model that connects observables such as neutrino luminosity and average energy with physical quantities. Here we show analytic solutions for the neutrino-light curve derived from the neutrino radiation transport equation by employing the diffusion approximation and the analytic density solution of the hydrostatic equation for the PNS. The neutrino luminosity and the average energy as functions of time are explicitly presented, with dependence on PNS mass, radius, the total energy of neutrinos, surface density, and opacity. The analytic solutions provide good representations of the numerical models from a few seconds after the explosion and let our rough estimate of these physical quantities to be made from observational data.

scholarly journals Effects of Small-Scale Fluctuations of Neutrino Flux in Supernova Explosions

2005 ◽  
Vol 192 ◽  
pp. 309-314
Author(s):  
Hideki Madokoro ◽  
Tetsuya Shimizu ◽  
Yuko Motizuki
Keyword(s):  
Neutrino Flux ◽  
Explosion Energy ◽  
Small Scale ◽  
Core Collapse ◽  
Effective Mechanism ◽  
Core Collapse Supernova ◽  
Neutrino Radiation ◽  
Spherical Explosion ◽  
Supernova Explosions ◽  
Neutrino Luminosity

SummaryWe examine effects of small-scale fluctuations with angle in the neutrino radiation in core-collapse supernova explosions. As the mode number of fluctuations increases, the results approach those of spherical explosion. We conclude that global anisotropy of the neutrino radiation is the most effective mechanism of increasing the explosion energy when the total neutrino luminosity is given.

scholarly journals Aspherical supernova explosions

2003 ◽  
Vol 212 ◽  
pp. 387-394 ◽  
Author(s):  
Peter A. Höflich ◽  
Dietrich Baade ◽  
Alexei M. Khokhlov ◽  
Lifan Wang ◽  
J. Craig Wheeler
Keyword(s):  
Axial Symmetry ◽  
Radiation Transport ◽  
Core Collapse ◽  
Intermediate Mass ◽  
Low Velocity ◽  
Transport Models ◽  
Sn 1987A ◽  
Direct Observations ◽  
Supernova Explosions ◽  
New Evidence

Core collapse supernovae (SN) are the final stages of stellar evolution in massive stars during which the central region collapses, forms a neutron star (NS), and the outer layers are ejected. Recent explosion scenarios assumed that the ejection is due to energy deposition by neutrinos into the envelope, but detailed models do not produce powerful explosions. There is new and mounting evidence for an asphericity and, in particular, for axial symmetry in several supernovae which may be hard to reconcile within the spherical picture. This evidence includes the observed high polarization and its variation with time, pulsar kicks, high velocity iron-group and intermediate-mass elements material observed in remnants, direct observations of the debris of SN 1987A, etc. Some of the new evidence is discussed in more detail. To be in agreement with the observations, any successful mechanism must invoke some sort of axial symmetry for the explosion. We consider jet-induced/dominated explosions of core collapse supernovae. Our study is based on detailed 3-d hydrodynamical and radiation transport models. We find that the observations can be explained by low velocity, massive jets which stall well within the SN envelope. Such outflows may be produced by MHD-mechanisms, convective dominated accretion disks on the central object or asymmetric neutrino emissions. Asymmetric density/chemical distributions and, for SN 2002ap, off-center energy depositions have been identified as crucial for the interpretation of the polarization.

scholarly journals Core-Collapse Supernova Simulations including Neutrino Interactions from the Virial EOS

2017 ◽  
Vol 12 (S331) ◽  
pp. 107-112 ◽  
Author(s):  
Evan O’Connor ◽  
C. J. Horowitz ◽  
Zidu Lin ◽  
Sean Couch
Keyword(s):  
Neutral Current ◽  
Radiation Hydrodynamics ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Sn 1987A ◽  
Interaction Terms ◽  
Central Engine ◽  
Matter Interaction ◽  
Supernova Explosions ◽  
Protoneutron Star

AbstractCore-collapse supernova explosions are driven by a central engine that converts a small fraction of the gravitational binding energy released during core collapse to outgoing kinetic energy. The suspected mode for this energy conversion is the neutrino mechanism, where a fraction of the neutrinos emitted from the newly formed protoneutron star are absorbed by and heat the matter behind the supernova shock. Accurate neutrino-matter interaction terms are crucial for simulating these explosions. In this proceedings for IAUS 331, SN 1987A, 30 years later, we explore several corrections to the neutrino-nucleon scattering opacity and demonstrate the effect on the dynamics of the core-collapse supernova central engine via two dimensional neutrino-radiation-hydrodynamics simulations. Our results reveal that the explosion properties are sensitive to corrections to the neutral-current scattering cross section at the 10-20% level, but only for densities at or above ~1012 g cm−3.

scholarly journals Neutrino-driven supernova explosions powered by nuclear reactions

2011 ◽  
Vol 7 (S279) ◽  
pp. 365-366 ◽  
Author(s):  
K. Nakamura ◽  
T. Takiwaki ◽  
K. Kotake ◽  
N. Nishimura
Keyword(s):  
Nuclear Reactions ◽  
Reaction Network ◽  
Numerical Code ◽  
Core Collapse ◽  
Hydrodynamic Simulations ◽  
Energy Feedback ◽  
Heating And Cooling ◽  
Nuclear Burning ◽  
Supernova Explosions ◽  
Neutrino Luminosity

AbstractWe have investigated the revival of a shock wave by nuclear burning reactions at the central region of core-collapse supernovae. For this purpose, we performed hydrodynamic simulations of core collapse and bounce for 15 M⊙ progenitor model, using ZEUS-MP code in axi-symmetric coordinates. Our numerical code is equipped with a simple nuclear reaction network including 13 α nuclei form 4He to 56Ni, and accounting for energy feedback from nuclear reactions as well as neutrino heating and cooling. We found that the energy released by nuclear reactions is significantly helpful in accelerating shock waves and is able to produce energetic explosion even if the input neutrino luminosity is low.

scholarly journals Core Collapse Supernova Models and Nucleosynthesis

2013 ◽  
Vol 9 (S296) ◽  
pp. 27-36
Author(s):  
Ken'ichi Nomoto
Keyword(s):  
Big Bang ◽  
Elemental Abundance ◽  
Core Collapse ◽  
Solar Abundance ◽  
First Stars ◽  
Abundance Pattern ◽  
Core Collapse Supernova ◽  
Abundance Patterns ◽  
Supernova Explosions ◽  
The Big Bang

AbstractAfter the Big Bang, production of heavy elements in the early Universe takes place in the first stars and their supernova explosions. The nature of the first supernovae, however, has not been well understood. The signature of nucleosynthesis yields of the first supernovae can be seen in the elemental abundance patterns observed in extremely metal-poor stars. Interestingly, those abundance patterns show some peculiarities relative to the solar abundance pattern, which should provide important clues to understanding the nature of early generations of supernovae. We review the recent results of the nucleosynthesis yields of massive stars. We examine how those yields are affected by some hydrodynamical effects during the supernova explosions, namely, explosion energies from those of hypernovae to faint supernovae, mixing and fallback of processed materials, asphericity, etc. Those parameters in the supernova nucleosynthesis models are constrained from observational data of supernovae and metal-poor stars.

NEUTRINO OSCILLATION IN SUPERNOVA AND GRB NUCLEOSYNTHESIS

2008 ◽  
Vol 23 (17n20) ◽  
pp. 1409-1418 ◽  
Author(s):  
TOSHITAKA KAJINO ◽  
TAKAHIRO SASAQUI ◽  
TAKASHI YOSHIDA ◽  
WAKO AOKI
Keyword(s):  
Black Hole ◽  
Gamma Ray ◽  
Light Element ◽  
Core Collapse ◽  
Mass Hierarchy ◽  
Solar Abundance ◽  
Abundance Pattern ◽  
Mixing Angle ◽  
Normal Mass ◽  
Supernova Explosions

Neutrinos play the critical roles in nucleosyntheses of light-to-heavy mass elements in core-collapse supernovae (SNe). The light element synthesis is affected strongly by neutrino oscillations (MSW effect) through the ν-process in outer layers of supernova explosions. Specifically the 7 Li and 11 B yields increase by factors of 1.9 and 1.3 respectively in the case of large mixing angle solution, normal mass hierarchy, and sin 2 2θ13 = 2 × 10−3 compared to those without the oscillations. In the case of inverted mass hierarchy or nonadiabatic 13-mixing resonance, the increment of their yields is much smaller. We thus propose that precise constraint on mass hierarchy and sin 2 2θ13 is given by future observations of Li / B ratio or Li abundance in stars and presolar grains which are made from supernova ejecta. Gamma ray burst (GRB) nucleosynthesis in contrast is not affected strongly by thermal neutrinos from the central core which culminates in black hole (BH), although the effect of neutrinos from proto-neutron star prior to black hole formation is still unknown. We calculate GRB nucleosynthesis by turning off the thermal neutrinos and find that the abundance pattern is totally different from ordinary SN nucleosynthesis which satisfies the universality to the solar abundance pattern.

Neutrino emission from the collapse of ∼104 M⊙ Population III supermassive stars

2021 ◽  
Vol 508 (1) ◽  
pp. 828-841
Author(s):  
Chris Nagele ◽  
Hideyuki Umeda ◽  
Koh Takahashi ◽  
Takashi Yoshida ◽  
Kohsuke Sumiyoshi
Keyword(s):  
Dark Matter ◽  
Massive Star ◽  
Direct Detection ◽  
Mass Range ◽  
Core Collapse ◽  
Low Density ◽  
Large Radius ◽  
Neutrino Luminosity ◽  
Neutrino Background ◽  
Population Iii

ABSTRACT We calculate the neutrino signal from Population III supermassive star (SMS) collapse using a neutrino transfer code originally developed for core-collapse supernovae and massive star collapse. Using this code, we are able to investigate the SMS mass range thought to undergo neutrino trapping (∼104 M⊙), a mass range which has been neglected by previous works because of the difficulty of neutrino transfer. For models in this mass range, we observe a neutrino sphere with a large radius and low density compared to typical massive star neutrino spheres. We calculate the neutrino light curve emitted from this neutrino sphere. The resulting neutrino luminosity is significantly lower than the results of a previous analytical model. We briefly discuss the possibility of detecting a neutrino burst from an SMS or the neutrino background from many SMSs and conclude that the former is unlikely with current technology, unless the SMS collapse is located as close as 1 Mpc, while the latter is also unlikely even under very generous assumptions. However, the SMS neutrino background is still of interest as it may serve as a source of noise in proposed dark matter direct detection experiments.

Sign in / Sign up

Export Citation Format

Share Document