宇宙射线加速和射电超新星的伽马射线信号

A. Marcowith , M. Renaud , V. Dwarkadas , V. Tatischeff
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引用次数: 19

摘要

核心坍缩超新星(SNe)是宇宙中最极端的事件之一。众所周知,它们是速度最快(但非或中等相对论性)的激波之一。一旦它穿过恒星大气层,SN爆炸波就会在大质量恒星祖先的风中膨胀。在IIb型SNe中,它的祖先可能是一颗红超巨星(RSG),它的质量损失率很大,恒星风很慢,产生非常致密的星周介质。高速激波和高密度介质都是引发粒子快速加速和由加速过程本身驱动的快速增长的不稳定性的关键因素。以著名的SN 1993J为例,重新分析了SN突出后正向激波中粒子加速的效率。我们发现,由激波前沿加速的高能粒子驱动的等离子体不稳定性在日内时间尺度上增长。这种增长和非线性过程的相互作用,允许在冲击时磁场的快速放大,这可以解释从源的无线电监测推断出的磁场强度。根据放大过程的不稳定性,发现最大粒子能量达到1-10 PeV。我们推导了由质子-质子相互作用产生的次级粒子(伽马射线、轻子和中微子)的时间依赖粒子谱和相关强子特征。我们发现切伦科夫望远镜阵列(CTA)可以很容易地探测到像SN 1993J这样的天体,特别是在1 TeV以上的天体,而当前的切伦科夫望远镜(如H.E.S.S.)只能勉强探测到这类事件。伽玛射线信号在爆发后的第一周被对产生过程大量吸收。我们预测在10 TeV以上的低中微子通量,这意味着只有1 Mpc的km3net型望远镜可以探测到视界。最后讨论了其他类型SNe中控制粒子加速和伽马射线发射的基本参数。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Cosmic-ray acceleration and gamma-ray signals from radio supernovæ

Core collapse supernovae (SNe) are among the most extreme events in the universe. The are known to harbor among the fastest (but non- or midly-relativistic) shock waves. Once it has crossed the stellar atmosphere, the SN blast wave expands in the wind of the massive star progenitor. In type IIb SNe, the progenitor is likely a Red SuperGiant (RSG) star which has a large mass loss rate and a slow stellar wind producing a very dense circumstellar medium. A high velocity shock and a high density medium are both key ingredients to initiate fast particle acceleration, and fast growing instabilities driven by the acceleration process itself. We have reanalyzed the efficiency of particle acceleration at the forward shock right after the SN outburst for the particular case of the well-known SN 1993J. We find that plasma instabilities driven by the energetic particles accelerated at the shock front grow over intraday timescales. This growth, and the interplay of non-linear process, permit a fast amplification of the magnetic field at the shock, that can explain the magnetic field strengths deduced from the radio monitoring of the source. The maximum particle energy is found to reach 1–10 PeV depending on the instability dominating the amplification process. We derive the time dependent particle spectra and the associated hadronic signatures of secondary particles (gamma-ray, leptons and neutrinos) arising from proton proton interactions.

We find that the Cherenkov Telescope Array (CTA) should easily detect objects like SN 1993J in particular above 1 TeV, while current generation of Cherenkov telescopes such as H.E.S.S. could only marginaly detect such events. The gamma-ray signal is found to be heavily absorbed by pair production process during the first week after the outburst. We predict a low neutrino flux above 10 TeV, implying a detectability horizon with a KM3NeT-type telescope of 1 Mpc only. We finally discuss the essential parameters that control the particle acceleration and gamma-ray emission in other type of SNe.

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