Gravitational radiation from colliding compact stars Hydrodynamical calculations in two dimensions

Details Gravitational radiation from colliding compact stars Hydrodynamical calculations in two dimensions Gravitational radiation from colliding compact stars Hydrodynamical calculations in two dimensions

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...287..728g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 287, Dec. 15, 1984, p. 728-744.

Astronomy and Astrophysics

Astrophysics

19

Collisions, Hydrodynamic Equations, Neutron Stars, Stellar Gravitation, Stellar Radiation, Computerized Simulation, Flow Equations, Gravitational Collapse, Poisson Equation, Time Dependence

Scientific paper

Gravitational radiation from the head-on collision of two identical compact stars is calculated using a two-dimensional, time-dependent, Newtonian hydrodynamical code. The star fluid is treated in an adiabatic approximation, and all relativistic effects are ignored. Gravitational radiation is computed as a small perturbation using linearized theory. The efficiency with which collisions generate radiation is typically equal to or less than 0.1 percent for colliding 1.4-solar-mass neutron stars. The efficiency is a steeply increasing function of the degree of central compaction. These results indicate that neutron star collisions might be the most copious emitters of gravitational radiation among promising astrophysical sources. However, there may be no likely astrophysical events that generate radiation with order unity efficiency. The calculations are compared with previous one-dimensional studies (Shapiro, 1980) and serve as a useful limit in which to compare future fully relativistic treatments.

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