Shock waves near the Schwarzschild radius and stability limits for stars

Details Shock waves near the Schwarzschild radius and stability limits for stars Shock waves near the Schwarzschild radius and stability limits for stars

Jun 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997phrvd..55.7518s&link_type=abstract

Physical Review D (Particles, Fields, Gravitation, and Cosmology), Volume 55, Issue 12, 15 June 1997, pp.7518-7528

Physics

2

Exact Solutions, Relativistic Stars: Structure, Stability, And Oscillations

Scientific paper

We analyze the time dilation associated with the propagation of a shock wave that moves outward into a static fluid sphere in general relativity. In this way we investigate the possibility that a shock wave inside a star could supply the pressure required to hold up a highly collapsed static outer layer. In such a model, one would observe a highly redshifted, time-independent emissions spectrum during the time interval between the time when the shock wave is formed, and the time when it reaches the star surface. Our conclusion is that the time it takes a shock wave to pass through a surface layer and reach the surface of a star, as seen by an observer in the far field, is on the order of the total mass of the star times a function that tends to infinity as the outer boundary of the star tends to its Schwarzschild radius.

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