Precession and system parameters in early-type binary models for SS 433

Details Precession and system parameters in early-type binary models for SS 433 Precession and system parameters in early-type binary models for SS 433

Feb 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....94..327h&link_type=abstract

Astronomy and Astrophysics, vol. 94, no. 2, Feb. 1981, p. 327-332.

Astronomy and Astrophysics

Astronomy

21

Binary Stars, Precession, Stellar Models, X Ray Stars, Balmer Series, Black Holes (Astronomy), Hot Stars, Neutron Stars, Radial Velocity

Scientific paper

We consider binary models in which the beams of SS 433 emerge from the center of a supercritical accretion disk around a compact object. Assuming the disk to be "slaved", i.e. its precession to be induced by driven Newtonian precession of a misaligned early-type companion star, the following constraints on the system parameters are found:
(i) If the companion's rotation is close to synchronous, only binary periods of the order of I d are possible;
(ii) if the companion's rotation is 1.4 to 2 times faster than synchronous, also orbital periods of the order of 10 d are allowed.
In both cases, if the compact star is a neutron star - which we consider most likely -` the early-type star should have a mass ≲ 10 Msun, implying, in view of its Mυ ≦ -4m, that it is probably a Wolf-Rayet star. The presence of strong Balmer-line emission then implies that it is most probably a WN 7-9 star. If the compact star is an 8 Msun black hole, also companion masses in the range of O stars (20 Msun or more) are allowed. A discussion of the reported l3.t spectroscopic and 6.5 d photometric periodicities and their possible near 1 d and near 0.5 d aliases, respectively, shows that binary periods near 1 d, though less likely, might not yet be completely ruled out.

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