AI 中文总结
研究极快新星V1723 Sco的多波长光变曲线，基于自洽模型结合白矮星吸积情况，用自由-自由发射模型和黑体近似模型重现光变曲线，通过伽马射线探测时间与模型V峰值一致，支持激波形成机制并得出激波壳层光学薄的结论。
AI 中文摘要
基于完全自洽的新星爆发模型，我们分析了极快新星V1723 Sco的多波长光变曲线。时间拉伸方法得出V波段的距离模数为$(m - M)_V = 15.3\pm 0.2$。利用完全自洽的新星爆发模型结合吸积率为$\dot{M}_{\rm acc}=1\times 10^{-9} ~M_\odot$ yr$^{-1}$的1.25 $M_\odot$白矮星上的光学厚风，成功重现了V波段光变曲线及超软X射线光变曲线。首次GeV伽马射线探测的时间与模型V峰值时间几乎一致，支持了激波形成机制，得出激波壳层光学薄的结论。
英文摘要
We have analyzed multiwavelength light curves of the very fast nova V1723 Sco, based on our fully self-consistent nova explosion models. The time-stretching method gives the distance modulus in the $V$ band of $(m-M)_V = 15.3\pm 0.2$. Then the absolute $V$ magnitude reaches $M_{V,\rm max}= m_{V, \rm max} - (m-M)_V= 6.77 - 15.3\pm 0.2 = -8.5\pm 0.2$. Using our fully self-consistent nova outburst model combined with the optically thick winds on a $1.25 ~M_\odot$ white dwarf accreted by a mass accretion rate of $\dot{M}_{\rm acc}=1\times 10^{-9} ~M_\odot$ yr$^{-1}$, we successfully reproduce the overall $V$ light curve with a free-free emission model as well as the supersoft X-ray light curve with a blackbody approximation model. The epoch of the first GeV gamma-ray detection is almost coincident with the epoch of our model $V$ peak. This supports the shock formation mechanism that a strong shock arises soon after the optical $V$ maximum far outside the WD photosphere. We conclude that the shocked shell is optically thin.
Comments17 pages, 7 figures, accepted for publication in ApJ
