COLLIMATED EMISSION FROM SS-433 - MODELING THE PROFILES OF THE MOVINGLINES

Profiles of the Halpha emission line produced in the jets of SS 433 ar e modeled under the assumption that the jets are heated by collimated x-ray emission from the accretion disk. It is shown that the position of a jet in the cone of that emission varies as a function of the obse rvation time, which can affect the appearance of the profiles. From th e modeling we estimate the lower limit of the opening angle of the emi ssion cone to be theta(c) greater-than-or-equal-to 14-degrees, and we show that the shape of the profiles is consistent with the proposed mo del of jet heating. The required luminosity of the collimated emission is L(c) greater than or similar to 3.10(39) erg/sec.