On the observability of spiral structures in CV accretion discs

Details On the observability of spiral structures in CV accretion discs On the observability of spiral structures in CV accretion discs

1999-02-25

arxiv.org/abs/astro-ph/9902358v1

Astronomy and Astrophysics

Astrophysics

Latex file, 12 pages, 9 figures, accepted for publication in Monthly Notices RAS

Scientific paper

10.1046/j.1365-8711.1999.02634.x

We use the grid of hydrodynamic accretion disc calculations of Stehle (1999) to construct orbital phase dependent emission line profiles of thin discs carrying spiral density waves. The observational signatures of spiral waves are explored to establish the feasibility of detecting spiral waves in cataclysmic variable discs using prominent emission lines in the visible range of the spectrum. For high Mach number accretion discs (M = 15-30), we find that the spiral shock arms are so tightly wound that they leave few obvious fingerprints in the emission lines. Only a minor variation of the double peak separation in the line profile at a level of 8% is produced. For accretion discs in outburst (M = 5-20) however, the lines are dominated by the emission from an m=2 spiral pattern in the disc. We show that reliable Doppler tomograms of spiral shock patterns can be reconstructed provided that a signal to noise of at least 15, a wavelength resolution of 80 km/s and a time resolution of 50 spectra per binary orbit is achieved. We confirm that the observed spiral pattern in the disc of IP Pegasi can be reproduced by tidal density waves in the accretion disc and demands the presence of a large, hot disc, at least in the early outburst stages.

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