STABILITY OF GASEOUS STARS IN THE NON-ISENTROPIC CASE  

作　　者：邓引斌 巴娜 谢华朝 

机构地区：[1]School of Mathematics and Statistics, Huazhong Normal University

出　　处：《Acta Mathematica Scientia》2010年第4期1347-1356,共10页数学物理学报（B辑英文版）

基　　金：supported by NSFC (10631030);the fund of CCNU for Ph.D Students (2009021)

摘　　要：The motion of the self-gravitational gaseous stars can be described by the Euler-Poisson equations. The main purpose of this article is concerned with the nonlinear stability of gaseous stars in the non-isentropic case, when 34 γ2, S（x,t） is a smooth bounded function. First, we verify that the steady states are minimizers of the energy via concentration-compactness method; then using the variational approach we obtain the stability results of the non-isentropic flow.The motion of the self-gravitational gaseous stars can be described by the Euler-Poisson equations. The main purpose of this article is concerned with the nonlinear stability of gaseous stars in the non-isentropic case, when 34 γ2, S（x,t） is a smooth bounded function. First, we verify that the steady states are minimizers of the energy via concentration-compactness method; then using the variational approach we obtain the stability results of the non-isentropic flow.

关 键 词：Euler-Poisson equations non-isentropic STABILITY 

分 类 号：O236[理学—运筹学与控制论]