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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Non-Thermal Radio and Gamma-Ray Emissions from a Supernova Remnant by Blast Wave Breaking Out of the Circumstellar Matter
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Non-Thermal Radio and Gamma-Ray Emissions from a Supernova Remnant by Blast Wave Breaking Out of the Circumstellar Matter

机译：超新星残余物的非热无线电和伽马射线辐射，其爆炸波冲出了星际物质

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We calculated synchrotron radio emission and γ-ray emission due to bremsstrahlung, inverse-Compton scattering, and π~0-decay from the remnant of supernova that exploded in the circumstellar matter (CSM) formed by the progenitor’s stellar wind. This sort of situation is a possible origin of mixed-morphology supernova remnants (SNRs), like W49B, which exhibit recombination-radiation spectra in X-ray emission. We assumed that the CSM of 1.5M_☉ exists at 0.07–3 pc away from the supernova in the interstellar medium (ISM) of density 0.016 cm~(-3). When the blast wave breaks out of the CSM into the ISM, its velocity rapidly increases, and hence particle acceleration is enhanced. The maximum energy of protons reaches ~1300 TeV just after the break-out with ~0.5% of the explosion energy. We considered the non-thermal emission from the blast-shocked ISM shell after the breakout. Synchrotron radio flux at 1 GHz is tens of Jy, comparable to that observed from mixed-morphology SNRs. Because of low density, the γ-ray luminosity is dominated by inverse-Compton scattering, which is higher than the π~0-decay luminosity by an order of magnitude. The total γ-ray luminosity, including bremsstrahlung, is on the order of 10~(33) erg s~(-1) lower than the typical value of 10~(35)–10~(36) erg s~(-1) observed from mixed-morphology SNRs. However, if, e.g., ~10% of accelerated protons interact with some matter of density of ~100 cm~(-3), the π~0-decay γ-ray luminosity would be enhanced to be comparable with the observed value.
机译：我们计算了由于致辐射，逆康普顿散射和超新星的残余而产生的同步辐射发射和γ射线辐射，这些超新星在由祖先的恒星风形成的星际物质（CSM）中爆炸。这种情况可能是混合形态的超新星遗迹（SNR）（如W49B）的可能起源，它在X射线发射中表现出重组辐射光谱。我们假设在密度为0.016 cm〜（-3）的星际介质（ISM）中，距超新星0.07–3 pc处存在1.5M_☉的CSM。当爆炸波从CSM爆发进入ISM时，其速度迅速增加，因此粒子加速度得到了增强。爆炸后，质子的最大能量达到约1300 TeV，约为爆炸能量的0.5％。我们考虑了爆炸后ISM爆炸壳产生的非热辐射。 1 GHz的同步加速器无线电通量为数十Jy，与从混合形态SNR观察到的相当。由于密度低，γ射线的光度主要由反康普顿散射控制，它比π〜0衰减的光度高一个数量级。包括致辐射在内的总γ射线光度比典型值10〜（35）–10〜（36）erg s〜（-1）低10〜（33）erg s〜（-1）数量级。 ）从混合形态SNR观察到。但是，例如，如果约10％的加速质子与约100 cm〜（-3）的密度发生相互作用，则π〜0衰变的γ射线发光度将提高到与观测值相当。

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