局域宇宙中超大质量恒星热过程的中微子发射
The neutrino emission from thermal processes in very massive stars in the local universe
摘要：
我们提出了一个新的概述非常大质量的恒星（VMS）的生活在中微子发射的热过程：对湮灭，等离子体衰变，光中微子过程，韧致辐射和重组过程中的燃烧阶段的选定VMS模型。我们使用的温度，密度，电子分数和核各向同性组成的VMS的现实条件。结果提出了一组祖星质量为150，200和300 M $_\odot$ Z=0.002和500 M $_\odot$ Z=0.006旋转模型，预计爆炸作为一对不稳定超新星在其生命的结束，除了300 M $_\odot$将最终作为一个黑洞。结果表明，对于VMS，由于初始温度和密度较高，热中微子发射早在氢燃烧阶段末期就已发生。利用模型各燃烧阶段的结构轮廓，计算了中微子的总发射率$Q_ν$和光度$L_ν$，观测到了光中微子在燃烧早期（H和He）的贡献和对湮灭在燃烧后期的贡献。对湮灭和光中微子过程是VMS演化过程中最主要的中微子能量损失机制。在O燃烧阶段，中微子的光度$\sim 10^{47-48}$ erg/s取决于它们的初始质量和金属丰度，略高于大质量恒星的中微子光度。这可能会揭示利用中微子探测来定位我们本地宇宙中对不稳定超新星候选者的可能性。
英文摘要：
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, $Q_ν$ and luminosity, $L_ν$ 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.
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