论文标题
新星爆发期间的强烈冲击：光谱和高能量排放中多个速度系统的起源
A strong shock during a nova outburst: an origin of multiple velocity systems in optical spectra and of high-energy emissions
论文作者
论文摘要
我们基于完全自洽的NOVA爆炸模型，提出了经典NOVAE中吸收/发射线系统的理论解释。我们发现，反向冲击远远超出了光球（$ \ gtrsim 10^{13} $ cm），因为较晚的质量具有更快的速度与早期发射的物质相撞。光学上的厚风以$ \ sim 10^{ - 4} 〜m_ \ odot $ yr $^{ - 1} $接近光学最大值的速度连续吹，但其速度降低到光学上的最大值并随后增加，因此仅在光学最大值后才出现冲击。 Nova弹射器将冲击分为三个部分，最外面的气体（最大风之前最早的风），震惊的壳和内部快风，分别有助于最大最大最大，主体和扩散增强的吸收/发射线系统。 Nova弹射器的很大一部分最终仅限于震惊的外壳。主系统的外观与冲击的出现一致。这种冲击足以解释热X射线排放。冲击层的高温为$ k t _ {\ rm sh} \ sim 1 $ kev $ \ times（（（v _ {\ rm wind} - v _ {\ rm shock}）/{\ rm 1000〜km〜km〜s}} - v _ {\ rm p}）/{\ rm 1000〜km〜s}^{ - 1}）^2 $，其中$ v _ {\ rm d} - v _ {\ rm p} $是diffuse -enhanced（$ v _ _} $ v _ {$ rm d {\ rm d {\ rm d（\ rm d（\ rm d}）的速度差P} $）系统。我们将1.3 $ m_ \ odot $白色矮人模型与GEV伽马射线检测到的经典NOVA V5856 SGR（ASASSN-16MA）的观察性质进行了比较，并讨论哪种Novae可以产生GEV GAMA-RAY的排放。
We propose a theoretical explanation of absorption/emission line systems in classical novae based on a fully self-consistent nova explosion model. We found that a reverse shock is formed far outside the photosphere ($\gtrsim 10^{13}$ cm) because later-ejected mass with a faster velocity collides with earlier-ejected matter. Optically thick winds blow continuously at a rate of $\sim 10^{-4} ~M_\odot$ yr$^{-1}$ near the optical maximum, but its velocity decreases toward the optical maximum and increases afterward, so that the shock arises only after the optical maximum. The nova ejecta is divided by the shock into three parts, the outermost expanding gas (earliest wind before maximum), shocked shell, and inner fast wind, which respectively contribute to pre-maximum, principal, and diffuse-enhanced absorption/emission line systems. A large part of nova ejecta is eventually confined to the shocked shell. The appearance of the principal system is consistent with the emergence of a shock. This shock is strong enough to explain thermal hard X-ray emissions. The shocked layer has a high temperature of $k T_{\rm sh} \sim 1$ keV $\times ((v_{\rm wind} - v_{\rm shock})/{\rm 1000 ~km~s}^{-1})^2 ={\rm 1 ~keV}\times ((v_{\rm d} - v_{\rm p})/{\rm 1000 ~km~s}^{-1})^2$, where $v_{\rm d} - v_{\rm p}$ is the velocity difference between the diffuse-enhanced ($v_{\rm d}$) and principal ($v_{\rm p}$) systems. We compare a 1.3 $M_\odot$ white dwarf model with the observational properties of the GeV gamma-ray detected classical nova V5856 Sgr (ASASSN-16ma) and discuss what kind of novae can produce GeV gamma-ray emissions.
