The neutrino emission from thermal processes in very massive stars in the local universe

Abstract

We present a new overview of the life of very massive stars (VMS) in terms of neutrino emission from thermal processes: pair annihilation, plasmon decay, photoneutrino process, bremsstrahlung and recombination processes in burning stages of selected VMS models. We use the realistic conditions of temperature, density, electron fraction and nuclear isotropic composition of the VMS. Results are presented for a set of progenitor stars with mass of 150, 200 and 300 M${}_{\odot }$ Z=0.002 and 500 M${}_{\odot }$ Z=0.006 rotating models which are expected to explode as a pair instability supernova at the end of their life except the 300 M${}_{\odot }$ would end up as a black hole. It is found that for VMS, thermal neutrino emission occurs as early as towards the end of hydrogen burning stage due to the high initial temperature and density of these VMS. We calculate the total neutrino emissivity, $Q_{\nu }$ and luminosity, $L_{\nu }$ using the structure profile of each burning stages of the models and observed the contribution of photoneutrino at early burning stages (H and He) and pair annihilation at the advanced stages. Pair annihilation and photoneutrino processes are the most dominant neutrino energy loss mechanisms throughout the evolutionary track of the VMS. At the O-burning stage, the neutrino luminosity $\sim 10^{47-48}$ erg/s depending on their initial mass and metallicity are slightly higher than the neutrino luminosity from massive stars. This could shed light on the possibility of using detection of neutrinos to locate the candidates for pair instability supernova in our local universe.

arXiv comment12 pages, submitted to MNRAS

References in corpus (28)

• How Massive Single Stars End their Life
• Mass-loss predictions for O and B stars as a function of metallicity
• Grids of stellar models with rotation - I. Models from 0.8 to 120 Msun at solar metallicity (Z = 0.014)
• An eclipsing binary distance to the Large Magellanic Cloud accurate to 2 per cent
• The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 Msun stellar mass limit
• Pair-Instability Supernovae, Gravity Waves, and Gamma-Ray Transients
• Supernova 2007bi as a pair-instability explosion
• Pair Instability Supernovae: Light Curves, Spectra, and Shock Breakout
• Evolution and fate of very massive stars
• Neutrino Energy Loss from the Plasma Process at all Temperatures and Densities
• The Destruction of Cosmological Minihalos by Primordial Supernovae
• Super-luminous supernovae at redshifts of 2.05 and 3.90
• Uncovering the Chemical Signature of the First Stars in the Universe
• Neon Abundances in B-Stars of the Orion Association: Solving the Solar Model Problem?
• Detection possibility of the pair-annihilation neutrinos from the neutrino-cooled pre-supernova star
• Neutrinos from beta processes in a presupernova: probing the isotopic evolution of a massive star
• Pair-Instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves
• Neutrino emissions in all flavors up to the pre-bounce of massive stars and the possibility of their detections
• Presupernova neutrino events relating to the final evolution of massive stars
• Presupernova neutrinos: realistic emissivities from stellar evolution
• Pair-Instability Supernovae in the Local Universe
• Neutrino energy loss rate in a stellar plasma
• Mass loss of massive stars near the Eddington luminosity by core neutrino emission shortly before their explosion
• On Stellar Evolution In A Neutrino Hertzsprung-Russell Diagram
• Spectra and rates of bremsstrahlung neutrino emission in stars
• The Neutrino Signal From Pair Instability Supernovae
• Pulsational Pair-instability Supernovae. II. Neutrino Signals from Pulsations and their Detection by Terrestrial Neutrino Detectors
• Supernova Model Discrimination with Hyper-Kamiokande

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• Stellar Neutrino Emission Across The Mass-Metallicity Plane
• Quasi-Sterile Neutrinos from Dark Sectors I. BSM matter effects in neutrino oscillations and the short-baseline anomalies
• Evolutionary models for the Very Massive Stars in the R136 cluster of 30 Doradus in the Large Magellanic Cloud