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29 March 2024
 
  » arxiv » 1704.8166

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The Spectrum of SS 433 in the H and K Bands
E.L. Robinson ; C.S. Froning ; D.T. Jaffe ; K.F. Kaplan ; H. Kim ; G.N. Mace ; K.R. Sokal ; J.-J. Lee ;
Date 26 Apr 2017
AbstractSS~433 is an X-ray binary and the source of sub-relativistic, precessing, baryonic jets. We present high-resolution spectrograms of SS 433 in the infrared H and K bands. The spectrum is dominated by hydrogen and helium emission lines. The precession phase of the emission lines from the jet continues to be described by a constant period, P_jet= 162.375 d. The limit on any secularly changing period is $|dot P| lesssim 10^{-5}$. The He I 2.0587 micron line has complex and variable P Cygni absorption features produced by an inhomogeneous wind with a maximum outflow velocity near 900 km/s. The He II emission lines in the spectrum also arise in this wind. The higher members of the hydrogen Brackett lines show a double-peaked profile with symmetric wings extending more than +/-1500 km/s from the line center. The lines display radial velocity variations in phase with the radial velocity variation expected of the compact star, and they show a distortion during disk eclipse that we interpret as a rotational distortion. We fit the line profiles with a model in which the emission comes from the surface of a symmetric, Keplerian accretion disk around the compact object. The outer edge of the disk has velocities that vary from 110 to 190 km/s. These comparatively low velocities place an important constraint on the mass of the compact star: Its mass must be less than 2.2 M_solar and is probably less than 1.6 M_solar.
Source arXiv, 1704.8166
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