Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...280..141r&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 280, no. 1, p. 141-156
Astronomy and Astrophysics
Astrophysics
6
Astronomical Models, Binary Stars, Collisions, Computerized Simulation, Hydrodynamics, Main Sequence Stars, Three Dimensional Models, White Dwarf Stars, Angular Momentum, Fast Fourier Transformations, Flow Theory, Mass Flow, Mass Transfer, Mathematical Models, Shock Waves
Scientific paper
We investigate the three-dimensional hydrodynamic evolution of a collision between a 0.5 solar mass white dwarf (modeled as gravitating impermeable sphere) and a 0.5 solar mass main-sequence star (modeled as polytrope with index n = 1.5). Self-gravity is included by calculating the potential through fast FOURIER transforms on equidistant CARTESIAN grids (number of zones: 323 and 643. The hydrodynamics is modeled by the 'Piecewise Parabolic Method' (PPM). The initial separation of the stars is two stellar radii and they approach each other on parabolic orbits. No energy sources (nuclear burning) or sinks (radiation, conduction) are included. The resolution in the vicinity of the white dwarf is increased by multiply nesting nine grids around the white dwarf, each finer grid being a factor of two smaller than the next coarser grid. The total dynamic range (size of the largest grid to size of the finest zone) is 8192 and 16384. This allows us to include a coarse model for the surface of the white dwarf (impermeable sphere) on the finest grid while at the same time evolving a main-sequence star on the coarser grids. In the highly dynamic evolution of central and non-central collisions (impact parameters: 0, 0.25 and 0.5 main-sequence star radii) the main-sequence star is disrupted and forms a disk. Comparisons with earlier calculations shows that the white dwarf surface can have a large influence in forming the flow white at the same time not significantly changing global values (e.g. total energy). However, the amount of matter unbound and angular momentum transfered are highly dependent on the model for the white dwarf.
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