A versatile numerical method for obtaining structures of rapidly rotating baroclinic stars: self-consistent and systematic solutions with shellular-type rotation
A versatile numerical method for obtaining structures of rapidly rotating baroclinic stars: self-consistent and systematic solutions with shellular-type rotation
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一种获得快速旋转斜压恒星结构的通用数值方法：壳状旋转的自洽系统解
DOI：
10.1093/mnras/stv2175
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发表时间：
2015
影响因子：
4.8
通讯作者：
K. Fujisawa
中科院分区：
文献类型：
--
作者：
K. Fujisawa
本文开发了一种基于自洽场方案获得快速旋转恒星结构的新颖数值方法。迭代获得解决方案。使用该方法可以自洽地计算快速旋转的正压和斜压平衡状态。通过改变恒星内部的等熵表面来研究两种类型的旋转斜斜恒星。系统地计算了这些解序列，并获得了不存在旋转平衡状态的临界旋转模型。所有这些旋转的斜压恒星都必然满足比耶克内斯-罗斯兰规则。如果假设恒星是理想气星，则可以成功获得具有壳状旋转的斜压星的自洽解，其中等熵表面是扁球形的，并且两极的表面温度比赤道的表面温度高。这些是具有壳状旋转的快速旋转斜斜恒星的第一个自洽和系统的解决方案。由于它们由于快速旋转而满足稳定性标准，因此这些旋转的斜压恒星将是动态稳定的。这种新颖的数值方法和快速旋转斜压恒星的解将有助于研究快速旋转的恒星演化。
This paper develops a novel numerical method for obtaining structures of rapidly rotating stars based on a self-consistent field scheme. The solution is obtained iteratively. Both rapidly rotating barotropic and baroclinic equilibrium states are calculated self-consistently using this method. Two types of rotating baroclinic stars are investigated by changing the isentropic surfaces inside the star. Solution sequences of these are calculated systematically and critical rotation models beyond which no rotating equilibrium state exists are also obtained. All of these rotating baroclinic stars satisfy necessarily the Bjerknes-Rosseland rules. Self-consistent solutions of baro-clinic stars with shellular-type rotation are successfully obtained where the isentropic surfaces are oblate and the surface temperature is hotter at the poles than at the equator if it is assumed that the star is an ideal gas star. These are the first self-consistent and systematic solutions of rapidly rotating baroclinic stars with shellular-type rotations. Since they satisfy the stability criterion due to their rapid rotation, these rotating baroclinic stars would be dynamically stable. This novel numerical method and the solutions of the rapidly rotating baroclinic stars will be useful for investigating stellar evolution with rapid rotations.