Turning point principle for relativistic stars
arXiv:2006.09749 · doi:10.1007/s00220-021-04197-6
Abstract
Upon specifying an equation of state, spherically symmetric steady states of the Einstein-Euler system are embedded in 1-parameter families of solutions, characterized by the value of their central redshift. In the 1960's Zel'dovich [50] and Wheeler [22] formulated a turning point principle which states that the spectral stability can be exchanged to instability and vice versa only at the extrema of mass along the mass-radius curve. Moreover the bending orientation at the extrema determines whether a growing mode is gained or lost. We prove the turning point principle and provide a detailed description of the linearized dynamics. One of the corollaries of our result is that the number of growing modes grows to infinity as the central redshift increases to infinity.
arXiv comment33 pages, 1 figure
References in corpus (17)
- Stability and Critical Phenomena of Black Holes and Black Rings
- General Relativistic Stars : Polytropic Equations of State
- A numerical investigation of the stability of steady states and critical phenomena for the spherically symmetric Einstein-Vlasov system
- Spherically symmetric relativistic stellar structures
- A non-variational approach to nonlinear stability in stellar dynamics applied to the King model
- Thermodynamical instabilities of perfect fluid spheres in General Relativity
- Black hole instabilities and local Penrose inequalities
- Dynamic and Thermodynamic Stability of Relativistic, Perfect Fluid Stars
- Spherically symmetric equilibria for self-gravitating kinetic or fluid models in the non-relativistic and relativistic case - A simple proof for finite extension
- Turning Point Instabilities for Relativistic Stars and Black Holes
- Stability and instability of self-gravitating relativistic matter distributions
- (In)finiteness of Spherically Symmetric Static Perfect Fluids
- On the small redshift limit of steady states of the spherically symmetric Einstein-Vlasov system and their stability
- On Spherically Symmetric Solutions of the Einstein-Euler Equations
- Driven neutron star collapse: Type~I critical phenomena and the initial black hole mass distribution
- Mass-radius spirals for steady state families of the Vlasov-Poisson system
- Separable Hamiltonian PDEs and Turning point principle for stability of gaseous stars
Cited by in corpus (4)
- The relativistic Euler equations with a physical vacuum boundary: Hadamard local well-posedness, rough solutions, and continuation criterion
- A numerical stability analysis for the Einstein-Vlasov system
- Collisionless equilibria in general relativity: stable configurations beyond the first binding energy maximum
- Einstein-Vlasov system with equal-angular momenta in