场耗散和冷却对强磁化白矮星质量-半径关系的影响
Effect of field dissipation and cooling on the mass-radius relation of strongly magnetised white dwarfs
摘要：
我们研究了高磁化白矮星的光度抑制及其对质量半径关系和冷却演化的影响。基于磁场相对于引力能的影响，我们对辐射不透明度、静磁平衡和简并核状态方程的处理作了适当的修正，从而得到了这些恒星的结构性质。虽然在没有磁场的情况下，无论光度如何，都保持了白矮星的质量极限，但大约$10^{14}\, {\rm G}$的强中心场可以产生质量高达$1.9\, M_{\odot}$的超白矮星白矮星。较小的白矮星在足够强的中心磁场下，即使它们的光度被显著地抑制到$10^{-16}\ L_{\odot}$，它们也倾向于保持超白矮星。由于$10\ {\rm Gyr}$上的冷却演化和同步的场衰减，小的磁化白矮星的极限质量可以随着时间的推移下降到$1.5\ M_{\odot}$。然而，这些系统中的大多数实际上仍然隐藏在整个冷却过程中，因为它们的高场和相应的低光度。利用恒星演化代码$\textit{STARS}$，我们获得了密切的协议与分析的质量极限估计，这表明我们的分析形式主义是物理动机。我们的结果表明，由于强场效应而诞生的超级钱德拉塞卡白矮星可能不会保持太久。这解释了它们的明显稀缺性，以及由于它们的亮度被抑制而难以检测。
英文摘要：
We investigate the luminosity suppression and its effect on the mass-radius relation as well as cooling evolution of highly magnetised white dwarfs. Based on the effect of magnetic field relative to gravitational energy, we suitably modify our treatment of the radiative opacity, magnetostatic equilibrium and degenerate core equation of state to obtain the structural properties of these stars. Although the Chandrasekhar mass limit is retained in the absence of magnetic field and irrespective of the luminosity, strong central fields of about $10^{14}\, {\rm G}$ can yield super-Chandrasekhar white dwarfs with masses up to $1.9\, M_{\odot}$. Smaller white dwarfs tend to remain super-Chandrasekhar for sufficiently strong central fields even when their luminosity is significantly suppressed to $10^{-16}\ L_{\odot}$. Owing to the cooling evolution and simultaneous field decay over $10\ {\rm Gyr}$, the limiting masses of small magnetised white dwarfs can fall to $1.5\ M_{\odot}$ over time. However the majority of these systems still remain practically hidden throughout their cooling evolution because of their high fields and correspondingly low luminosities. Utilising the stellar evolution code $\textit{STARS}$, we obtain close agreement with the analytical mass limit estimates and this suggests that our analytical formalism is physically motivated. Our results argue that super-Chandrasekhar white dwarfs born due to strong field effects may not remain so for long. This explains their apparent scarcity in addition to making them hard to detect because of their suppressed luminosities.
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