对AM CVn与双爆轰超新星前身星双星系统CD-30$^{\circ}$11223的建模研究
Modelling the AM CVn and Double Detonation Supernova Progenitor Binary System CD-30$^{\circ}$11223
AI总结：
本研究利用MESA软件对双爆轰超新星前身星双星系统CD-30进行建模，发现0.47太阳质量的sdB解更优，证实其将在约55 Myr后爆发并抛射sdB，末期将呈现AM CVn型系统特征。
摘要：
我们利用开源恒星演化软件MESA，对CD-30$^{\circ}$11223（简称CD-30）进行了详细的建模研究。该系统是一个热亚矮星-白矮星双星系统，被确认为双爆轰超新星的前身星。我们重点实施了经过仔细调整的双星演化模型，以匹配包括$\log g$和$T_{\rm eff}$在内的系统观测特征。我们首次在建模过程中考虑了氢包层的结构，并发现引入元素扩散对于匹配观测到的半径和温度至关重要。我们研究了先前为该系统提出的两种sdB质量解（0.47和0.54 $M_{\odot}$），强烈倾向于0.47 $M_{\odot}$的解。我们使用模型将WD的冷却年龄与sdB的年龄进行了比较，结果表明sdB可能比WD更老，这与紧凑型sdB-WD双星系统的标准假设相反。随后，我们提出了CD-30的一种可能的替代形成渠道。我们还对该系统进行了双星演化建模，以研究质量转移、轨道周期演化和光度演化等多个方面。我们的模型证实CD-30是双爆轰超新星前身星，预计将在距今约55 Myr后爆发。WD吸积了约0.17 $M_{\odot}$厚的氦壳层并引发爆轰，导致一个0.30 $M_{\odot}$的sdB以约750 km/s的速度被抛射出去。该系统最后的15 Myr以氦吸积为特征，这一过程主导了系统的光度，可能类似于AM CVn型系统。
英文摘要：
We present a detailed modelling study of CD-30$^{\circ}$11223 (CD-30), a hot subdwarf (sdB)-white dwarf (WD) binary identified as a double detonation supernova progenitor, using the open-source stellar evolution software MESA. We focus on implementing binary evolution models carefully tuned to match the observed characteristics of the system including $\log g$ and $T_{\rm eff}$. For the first time, we account for the structure of the hydrogen envelope throughout the modelling, and find that the inclusion of element diffusion is important for matching the observed radius and temperature. We investigate the two sdB mass solutions (0.47 and 0.54 $M_{\odot}$) previously proposed for this system, strongly favouring the 0.47 $M_{\odot}$ solution. The WD cooling age is compared against the sdB age using our models, which suggest an sdB likely older than the WD, contrary to the standard assumption for compact sdB-WD binaries. Subsequently, we propose a possible alternate formation channel for CD-30. We also perform binary evolution modelling of the system to study various aspects such as mass transfer, orbital period evolution and luminosity evolution. Our models confirm CD-30 as a double detonation supernova progenitor, expected to explode $\approx55$ Myr from now. The WD accretes a $\approx0.17$ $M_{\odot}$ thick helium shell that causes a detonation, leaving a 0.30 $M_{\odot}$ sdB ejected at $\approx$750 km/s. The final 15 Myr of the system are characterised by helium accretion which dominates the system luminosity, possibly resembling an AM CVn-type system.
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