On the equations of thermally radiative magnetohydrodynamics
On the equations of thermally radiative magnetohydrodynamics
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DOI：
10.1016/j.jde.2014.06.015
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发表时间：
2014-11
影响因子：
2.4
通讯作者：
Xiaoli Li;B. Guo
中科院分区：
文献类型：
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作者：
Xiaoli Li;B. Guo
考虑了粘性可压缩热辐射磁流体动力学（MHD）流与自引力耦合的初边值问题，该问题描述了气态恒星在r3有界域中的动力学。给出了守恒边界条件。与Ducomet-Feireisl[13]（参见，例如，Feireisl [18], Feireisl-Novotný[20]）相比，本文给出了一个更一般的本构关系。分析考虑了真空条件下的初始密度。每个输运系数都有一定的温度标度。通过三阶逼近和弱收敛方法，证明了任意有限能量和有限熵数据下变分（弱）解的整体存在性。
An initial–boundary value problem is considered for the viscous compressible thermally radiative magnetohydrodynamic (MHD) flows coupled to self-gravitation describing the dynamics of gaseous stars in a bounded domain of R 3. The conservative boundary conditions are prescribed. Compared to Ducomet–Feireisl [13](also see, for instance, Feireisl [18], Feireisl–Novotný [20]), a rather more general constitutive relationship is given in this paper. The analysis allows for the initial density with vacuum. Every transport coefficient admits a certain temperature scaling. The global existence of a variational (weak) solution with any finite energy and finite entropy data is established through a three-level approximation and methods of weak convergence.