论文标题
首先在古典Novae中观察到的X射线闪光灯的轻曲线分析
A light-curve analysis of the X-ray flash first observed in classical novae
论文作者
论文摘要
X射线闪光灯预计在Nova爆发的早期阶段，最终用{\ it srg}/Erosita在经典的Nova YZ Eticuli 2020中被检测到。观察到的闪存时间尺度，亮度，黑体温度和黑体温度极大地限制了NOVA模型。我们提出了各种白色矮人（WD）质量和质量积聚率的X射线闪光灯的光曲线模型。我们发现Yz RET中的WD质量与$ M _ {\ rm WD} \ SIM 1.3〜M_ \ ODOT $，质量增值率为$ \ dot M _ {\ rm acc} \ sim Acc} \ sim 5 \ sim 5 \ sim 5 \ sim 5 \ times 10^{ - 10} - 10} - 10} - 5 \ 5 \ 5 \ 5 \ times 10^} $ yr质量积聚率在它们之间发生变化，以与{\ it srg}/rotosita观察一致。 X射线观察证实了在X射线闪光灯处的光度接近Eddington限制。光光度半径超过$ \ sim 0.1〜r_ \ odot $的出现，通过强吸收终止了Yz RET的X射线闪光灯。这对风质量损失的起始时间设定了约束。核心材料对富氢包膜的略有污染似乎是解释X射线闪光的持续时间很短的。
An X-ray flash, expected in a very early phase of a nova outburst, was at last detected with the {\it SRG}/eROSITA in the classical nova YZ Reticuli 2020. The observed flash timescale, luminosity, and blackbody temperature substantially constrain the nova model. We present light curve models of the X-ray flash for various white dwarf (WD) masses and mass accretion rates. We have found the WD mass in YZ Ret to be as massive as $M_{\rm WD}\sim 1.3 ~M_\odot$ with mass accretion rates of $\dot M_{\rm acc}\sim 5 \times 10^{-10}- 5\times 10^{-9} ~M_\odot$ yr$^{-1}$ including the case that the mass accretion rate is changing between them, to be consistent with the {\it SRG}/eROSITA observation. The X-ray observation confirms the luminosity to be close to the Eddington limit at the X-ray flash. The occurrence of optically thick winds, with the photospheric radius exceeding $\sim 0.1~R_\odot$, terminated the X-ray flash of YZ Ret by strong absorption. This sets a constrain on the starting time of wind mass loss. A slight contamination of the core material into the hydrogen rich envelope seems to be preferred to explain a very short duration of the X-ray flash.
