Beam models for SS 433

Details Beam models for SS 433 Beam models for SS 433

Jun 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...238..722b&link_type=abstract

Astrophysical Journal, Part 1, vol. 238, June 1, 1980, p. 722-730.

Astronomy and Astrophysics

Astronomy

126

Binary Stars, Neutron Stars, Stellar Models, Variable Stars, Emission Spectra, Radio Sources (Astronomy), Stellar Evolution, Stellar Rotation, Stellar Spectra

Scientific paper

Observational constraints on the energetics of beam models of the emission line object SS 433 are examined, and a likely astrophysical model is derived. Consideration is given to the main spectral features of the object, which exhibits red- and blue-shifted emission line systems which oscillate across the spectrum with large amplitudes, and the constraints these features impose on the two collimated gaseous streams emerging in opposite directions from a central object and precessing with a period of 164 days thought to be responsible for the shifted lines are discussed. Specific models for the excitation of the line-emitting gas are examined, and it is shown that excitation by shock-produced X-rays and EUV can account for most of the general features of the SS 433 spectrum. The action of the beams is discussed as the source of the supernovae remnant-like radio source W 50, on which SS 433 is centered. It is suggested that SS 433 contains a neutron star, and that the 164-day period and the geometry of the oscillations in beam direction can be explained by the geodetic precession of the rapidly rotating neutron star by a binary companion. Finally, the evolution of the system is discussed, and predictions of the model concerning the source spectrum and beam resolution are summarized.

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