Astrophysics and Space Science

, Volume 130, Issue 1–2, pp 351–364 | Cite as

Accretion disk structure in SS Cygni

  • F. V. Hessman
IV. Accretion Disks


High-resolution Coude observations of non-axisymmetric line emission from the dwarf nova SS Cygni are presented. By subtracting the constant line component, the asymmetric line emission responsible for the observed phase shift between the absorption and emission line radial velocity curves can be isolated. The extra emission is a large fraction of the total line emission and extends to large velocities (∼1500 km sec−1). The phase stability of the emission demands a large-scale structure which is fixed in the frame of the binary. A magnetic origin of the excitation cannot be ruled out but is implausible. A simple explanation is that the accretion stream from the companion star is able to spill over the edge of the disk, introducing emission at non-circular velocities and most likely disturbing the upper layers of the accretion disk.


Radial Velocity Line Emission Phase Stability Accretion Disk Simple Explanation 
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Copyright information

© D. Reidel Publishing Company 1987

Authors and Affiliations

  • F. V. Hessman
    • 1
  1. 1.Max-Planck-Institut für AstronomieHeidelbergF.R.G.

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