Shock breakout theory
Shock breakout theory
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DOI：
10.1007/978-3-319-21846-5_33
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发表时间：
2016-07
期刊：
影响因子：
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通讯作者：
E. Waxman;B. Katz
中科院分区：
文献类型：
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作者：
E. Waxman;B. Katz
最早的超新星 (SN) 发射是在激波前方等离子体的光学深度下降到 c/v 以下时产生的，其中 v 是激波速度。当冲击波到达恒星边缘时，可能会发生这种“爆发”，在几秒到不到一小时的时间尺度上产生明亮的X射线/紫外线闪光，然后在一天的时间尺度上从不断扩大的冷却包层中发出紫外线/光学“冷却”辐射。如果在爆炸前从祖星喷射出的星周物质（CSM）的光学深度大于c/v，则爆发将在CSM内更大的半径处发生，将其持续时间延长至数天的时间尺度。早期爆发和冷却发射的特性带有祖星结构（例如其半径和表面组成）及其质量损失历史的独特特征。广域瞬态勘测的最新进展使得超新星在一天时间范围内的检测成为可能，并被用来对所有类型的超新星祖先设置独特的约束。本章包括对SN突破理论的教学描述，对迄今为止我们从观测中学到的知识的简要概述，以及为了取得进一步重大进展所需的观测能力的进步。
The earliest supernova (SN) emission is produced when the optical depth of the plasma lying ahead of the shock, which ejects the envelope, drops below c/v, where v is the shock velocity. This "breakout" may occur when the shock reaches the edge of the star, producing a bright X-ray/UV flash on time scales of seconds to a fraction of an hour, followed by UV/optical "cooling" emission from the expanding cooling envelope on a day time-scale. If the optical depth of circumstellar material (CSM) ejected from the progenitor star prior to the explosion is larger than c/v, the breakout will take place at larger radii, within the CSM, extending its duration to days time scale. The properties of the early, breakout and cooling, emission carry unique signatures of the structure of the progenitor star (e.g. its radius and surface composition) and of its mass-loss history. The recent progress of wide-field transient surveys enable SN detections on a day time scale, and are being used to set unique constraints on the progenitors of SNe of all types. This chapter includes a pedagogical description of SN breakout theory, and a concise overview of what we have learned from observations so far, and of advances in observational capabilities that are required in order to make further significant progress.