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29 March 2024 |
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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 | Abstract: | SS~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 | Services: | Forum | Review | PDF | Favorites |
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