Gravitational radiation from a rotating collapsing gaseous ellipsoid

Details Gravitational radiation from a rotating collapsing gaseous ellipsoid Gravitational radiation from a rotating collapsing gaseous ellipsoid

Jun 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...214..576c&link_type=abstract

Astrophysical Journal, Part 1, vol. 214, June 1, 1977, p. 576-583.

Astronomy and Astrophysics

Astrophysics

14

Gravitational Collapse, Gravitational Waves, Stellar Evolution, Stellar Rotation, Angular Momentum, Energy Dissipation, Tables (Data)

Scientific paper

The collapse of a uniformly rotating and spatially homogeneous axisymmetric spheroid with internal gas pressure is followed numerically. Energy dissipation by gravitational radiation (GR) is calculated in the weak-field limit; the nonzero internal temperature allows parametrization of a 'thermal' energy loss in a crude attempt to model photon and neutrino losses. The amount of GR energy radiated and the details of the collapse process of a 1.4-solar mass white dwarf with initial density of 1 billion g/cu cm depend not only on the initial eccentricity, central temperature, and total angular momentum, but also strongly on thermal energy loss. While the total GR energy available lies in the range between 10 to the 44th power and 10 to the 50th power erg, the non-GR component can be much larger, resulting in a damping out of the collapse bounces when the free parameter in the expression for thermal energy loss is large. In general, the total GR energy from all the bounces is of the same order as that in all the preceding free falls. However, the last free fall may contribute a negligible to a significant portion of the total GR energy emitted.

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