Existence and uniqueness of rigidly rotating stars in second order perturbation theory

General Relativity, Geometry and Analysis: beyond the first 100 years after Einstein

08 October 10:00 - 11:00

Marc Mars - University of Salamanca

The Hartle-Thorne model describes slowly, rigidly rotating stars in the strong field regime by using perturbation theory up to second order. The model involves a number of hypotheses, some explicit and some implicit, on the structure and regularity of the perturbation tensors. In this talk I present work in collaboration with Reina and Vera where slowly, rigidly rotating fluid balls are analyzed consistently in second order perturbation theory by imposing only basic differentiability requirements. We prove in particular that, at this level of approximation, the spacetime is fully determined by two parameters, namely the central pressure and the rotation parameter of the fluid.
Lars Andersson
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
Mattias Dahl
KTH Royal Institute of Technology
Philippe G. LeFloch
Sorbonne University
Richard Schoen
University of California, Irvine


Mattias Dahl


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