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Stability of Rotating Gaseous Stars

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Abstract

We consider stability of rotating gaseous stars modeled by the Euler–Poisson system with general equation of states. When the angular velocity of the star is Rayleigh stable, we proved a sharp stability criterion for axi-symmetric perturbations. We also obtained estimates for the number of unstable modes and exponential trichotomy for the linearized Euler–Poisson system. By using this stability criterion, we proved that for a family of slowly rotating stars parameterized by the center density with fixed angular velocity, the turning point principle is not true. That is, unlike the case of non-rotating stars, the change of stability of the rotating stars does not occur at extrema points of the total mass. By contrast, we proved that the turning point principle is true for the family of slowly rotating stars with fixed angular momentum distribution. When the angular velocity is Rayleigh unstable, we proved linear instability of rotating stars. Moreover, we gave a complete description of the spectra and sharp growth estimates for the linearized Euler–Poisson system.

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Acknowledgements

This work is supported partly by the NSF Grants DMS-1715201 and DMS-2007457 (Lin) and the China Scholarship Council No. 201806310066 (Wang).

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Authors and Affiliations

  1. School of Mathematics, Georgia Institute of Technology, Atlanta, GA, 30332, USA

    Zhiwu Lin

  2. School of Mathematical Sciences, Peking University, Beijing, 100871, China

    Yucong Wang

  3. School of Mathematical Sciences, Xiamen University, Xiamen, 361005, China

    Yucong Wang

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  1. Zhiwu Lin
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  2. Yucong Wang
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Correspondence to Yucong Wang.

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Communicated by A. Ionescu.

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Lin, Z., Wang, Y. Stability of Rotating Gaseous Stars. Commun. Math. Phys. 402, 1725–1763 (2023). https://doi.org/10.1007/s00220-023-04763-0

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