经典新星YZ Ret的光变曲线分析：用完全自洽的新星爆发模型重新审视
Light-curve analysis of the classical nova YZ Ret: revisit with fully self-consistent nova outburst models
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中文总结 AI 辅助
本研究用完全自洽的新星爆发模型重新分析YZ Ret的多波段光变曲线，成功再现观测数据并解释GeV伽马射线发射的起源，揭示了激波形成机制。
中文摘要 AI 辅助
YZ Ret是一颗观测良好的新星，从经典新星中首次探测到X射线闪光阶段开始，直到超软X射线源阶段结束。我们重新分析了YZ Ret在整个爆发期间的多波段光变曲线。我们的完全自洽新星爆发模型，即一颗1.25太阳质量的白矮星（WD）和吸积率为1×10^-9太阳质量/年的WD吸积，合理地再现了V/g光变曲线以及极早期的X射线闪光和晚期的超软X射线光变曲线。该模型解释了GeV伽马射线发射的出现时代，因为激波自然地在光学极大之后产生于新星（WD）光球层之外很远的地方。在我们的模型中，在光学极大之前，后期抛射物质的速度小于早期抛射物的速度，因此抛射物膨胀；而在光学极大之后，后期抛射物质的速度大于早期抛射物的速度，与早期抛射物的碰撞产生激波。
英文摘要
YZ Ret is a well observed nova from the first detection of an X-ray flash phase in classical novae until the end of a supersoft X-ray source phase. We have reanalyzed multiwavelength light curves of YZ Ret over the total duration of the outburst. Our fully self-consistent nova outburst model, a 1.25 $M_\odot$ white dwarf (WD) and a mass accretion rate of $1\times 10^{-9} ~M_\odot$ yr$^{-1}$ on to the WD, reasonably reproduced $V$/$g$ light curves as well as the very early X-ray flash and late supersoft X-ray light curves. This model explains the emergence epoch of the GeV gamma-ray emission because a shock naturally arises far outside the nova (WD) photosphere just after the optical maximum. In our model, before optical maximum, later ejected matter has a smaller velocity than that of earlier ejecta and therefore the ejecta expands while, after optical maximum, later ejected matter has a larger velocity than that of earlier ejecta and collision with the earlier ejecta makes a shock.
发表机构
- The University of Tokyo（东京大学）
- Keio University（庆应义塾大学）
机构由 AI 辅助整理，请以论文原文为准。
