Acta mathematica scientia, Series B >
STABILITY OF GASEOUS STARS IN THE NON-ISENTROPIC CASE
Received date: 2008-09-22
Revised date: 2009-02-12
Online published: 2010-07-20
Supported by
Research was supported by NSFC (10631030) and the fund of CCNU for Ph.D Students (2009021)
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
4/3 < γ <2, 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.
Key words： Euler-Poisson equations; non-isentropic; stability
DENG Yin-Bin , BA Na , XIE Hua-Chao . STABILITY OF GASEOUS STARS IN THE NON-ISENTROPIC CASE[J]. Acta mathematica scientia, Series B, 2010 , 30(4) : 1347 -1356 . DOI: 10.1016/S0252-9602(10)60130-0
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