Supersonic wind accretion in massive close binary systems - A 3D SPH simulation of CEN X-3

Details Supersonic wind accretion in massive close binary systems - A 3D SPH simulation of CEN X-3 Supersonic wind accretion in massive close binary systems - A 3D SPH simulation of CEN X-3

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.295..618l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 295, p. 618

Astronomy and Astrophysics

Astronomy

15

Accretion Disks, Binary Stars, Stellar Models, Stellar Winds, Hydrodynamics, Three Dimensional Models, Supersonic Speed, Simulation

Scientific paper

We study the 3D SPH structure and dynamics of an accretion disk generated in a close binary system by supersonic wind accretion from a massive secondary onto a compact primary. The stellar masses and separation between the two components are characteristic of the Cen X-3 system: the secondary is a 19.1-solar-mass star not filling completely its Roche lobe, while the primary is a white dwarf or a neutron star of 1.4 solar mass. An interesting result of our simulation is that, in a quasi-stationary state attained after about four orbital periods, only about three-quarters of the particles released by the secondary penetrate the primary Roche lobe. The disk is remarkably elongated and thick, and consistent deviations from the 'standard model' of specific angular momentum and radial temperature distributions have been found. However, the most interesting result is that the azimuthal distribution of the radial Mach number shows oblique structures (spiral shocks), which persist from the outer edge to the inner regions, in contrast to the case of disks formed by the usual L1 accretion and even by wind accretion in much less massive systems.

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