The astrophysical torus. 2: Light curves of SS 433

Details The astrophysical torus. 2: Light curves of SS 433 The astrophysical torus. 2: Light curves of SS 433

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasj...45..727s&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 45, no. 5, p. 727-731

Astronomy and Astrophysics

Astronomy

8

Accretion Disks, Astronomical Models, Light Curve, Neutron Stars, Toruses, X Ray Binaries, Companion Stars, Early Stars, Gravitational Fields, Mass Ratios, Photometry, Radial Velocity

Scientific paper

Using the mass function obtained by D'Odorico et al. (1991), we recalculate the theoretical light curves of SS 433 in the primary eclipse and confront them with observations. We assume that in SS 433 there exists a geometrically thick torus around a compact object, and that the primary eclipse is an eclipse of the torus by a companion of an early-type star. The main parameters are the shape of the tori, the size of the tori, and the binary mass ratio. We obtain light curves for several combinations of parameters. The light curves for sufficiently thick tori are deep at the mid-eclipse and preferable, while those for geometrically thin tori are shallow. The duration of eclipse for a large torus is long and beneficial, while that for a small torus is short. Finally, Delta m at mid-eclipse for a thick torus around a neutron star becomes approximately 0.6 and suitable, whereas for thick tori around a black hole it is approximately 0.3. Hence, under the new mass function, geometrically thick and wide tori around a neutron star can well reproduce the observed light curves of SS 433.

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