Hydrodynamic simulations of white dwarf-massive main-sequence star collisions in dense galactic nuclei

Details Hydrodynamic simulations of white dwarf-massive main-sequence star collisions in dense galactic nuclei Hydrodynamic simulations of white dwarf-massive main-sequence star collisions in dense galactic nuclei

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.227..967r&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 227, Aug. 15, 1987, p. 967-973.

Statistics

Computation

3

Galactic Nuclei, Hydrodynamics, White Dwarf Stars, Computational Astrophysics, Stellar Activity

Scientific paper

Physical collisions between stars should occur very frequently in the dense nuclei of galaxies, and probably change the luminosity and luminosity function there significantly. Collisions between main-sequence stars are coalescent at low velocities and disruptive at high velocity. Collisions between a white dwarf and low-mass or intermediate-mass (0.1-1 solar mass) main-sequence stars disrupt the latter, mostly due to the liberation of considerable amounts of nuclear energy. Hydrodynamic simulations are used to demonstrate that significant disruption also occurs for a massive (about 10 solar mass) main-sequence star during a head-on collision with a white dwarf, but for a different reason. Much of the nondegenerate star's initial kinetic energy is stored as heat during a collapse episode on to a white dwarf. Then, the stored energy is converted back into kinetic energy as much of the main-sequence star is ejected in all directions by the unscathed white dwarf.

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