Gravitational radiation from colliding, compact stars - Hydrodynamic calculations in one dimension

Details Gravitational radiation from colliding, compact stars - Hydrodynamic calculations in one dimension Gravitational radiation from colliding, compact stars - Hydrodynamic calculations in one dimension

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...240..246s&link_type=abstract

Astrophysical Journal, Part 1, vol. 240, Aug. 15, 1980, p. 246-263.

Astronomy and Astrophysics

Astrophysics

7

Gravitational Waves, Hydrodynamics, Neutron Stars, Supermassive Stars, Collisions, Luminosity, Polytropic Processes, Stellar Models

Scientific paper

The gravitational radiation resulting from the head-on collision of two identical uncollapsed compact stars at free-fall velocity is calculated in terms of a one-dimensional hydrodynamical model. The dynamical motion is treated as strictly Newtonian, and gravitational radiation is calculated as a perturbation by the use of linearized theory in the slow-motion, weak-field approximation, with all motion assumed to be parallel to the collision axis. Analytical and numerical solutions are obtained and compared for the collision of cold, homogeneous, cubical stars in the absence of gravity in order to formulate reliable numerical procedures for the calculation of gravitational wave luminosities. Numerical consideration is then given to the head-on collision of identical planar polytropes, and total gravitational radiation efficiencies are calculated for the collisions of two neutron stars and two supermassive stars. The efficiencies are shown to be greater than 1% for neutron stars with masses greater than 0.5 solar masses and much less than 1% for supermassive star collisions involving stars with masses greater than 60 solar masses. Implications of the results for the detection of gravitational waves are considered.

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