The feasibility of observing spiral shocks in accretion disks

Details The feasibility of observing spiral shocks in accretion disks The feasibility of observing spiral shocks in accretion disks

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...232..371b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 232, no. 2, June 1990, p. 371-376. Research supported by DFG.

Astronomy and Astrophysics

Astrophysics

12

Accretion Disks, Cataclysmic Variables, Shock Waves, Astronomical Spectroscopy, Light Curve, Mach Number

Scientific paper

Angular momentum transport in accretion disks has been suggested to be due either to (turbulent or magnetic) viscosity or to spiral shocks. To investigate which observations can discriminate between these mechanisms, the spectrum and the eclipse light curve in the optical and ultraviolet wavelength ranges are calculated for disks that contain spiral shocks. It is concluded that the best signature of the presence of such shocks is an asymmetry in the ultraviolet eclipse light curve. Only relatively strong shocks can be expected to be detected.

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