Models of head-on collisions between a white dwarf and a low-mass main sequence star

Details Models of head-on collisions between a white dwarf and a low-mass main sequence star Models of head-on collisions between a white dwarf and a low-mass main sequence star

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...208...69r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 208, no. 1-2, Jan. 1989, p. 69-76. Research supported by the Max-Planck-Instit

Astronomy and Astrophysics

Astrophysics

9

Collisions, Main Sequence Stars, Stellar Mass, Stellar Models, White Dwarf Stars, Globular Clusters, Hydrodynamic Equations, Shock Wave Interaction, Stellar Mass Ejection

Scientific paper

Two-dimensional axisymmetric hydrodynamical calculations are performed to simulate the collision of a white dwarf of 0.5 solar mass with main sequence stars of 0.5 and 1.0 solar masses. A substantial amount of the main sequence star is dissipated in the collision; however the amount is dependent on its mass and on the initial velocity of the white dwarf. Although nuclear reactions were not included in the hydrodynamic calculations, detailed estimates of reaction rates, based upon the numerical results, indicate that shock heating is the dominant mechanism causing dissipation. The precise role of nuclear energy is not determined because of uncertainties arising from the approximations and the finite grid. In all calculated cases the amount of material captured by the white dwarf is sufficient so that it subsequently will evolve into a red giant.

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