CN Orionis - A touchstone for dwarf nova outburst models

Details CN Orionis - A touchstone for dwarf nova outburst models CN Orionis - A touchstone for dwarf nova outburst models

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...193..101m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 193, no. 1-2, March 1988, p. 101-112.

Astronomy and Astrophysics

Astrophysics

9

Cataclysmic Variables, Dwarf Novae, Stellar Models, Absorption Spectra, Accretion Disks, Astronomical Photometry, H Alpha Line, Stellar Color, Stellar Spectra

Scientific paper

The results of observations of the initial phase of a dwarf nova eruption of CN Orionis conducted to test dwarf nova outburst models are presented. No evidence for a distinct increase in the mass transfer rate prior to and simultaneously with the beginning of the outburst was found, contrary to the expectation of the transfer instability model. Hence the only existing alternative, the disk instability model, is favored. The variability of the period of the principal hump cannot be attributed to the orbital motion only, and must be explained in terms of the stream penetration effect. A beat phenomenon of the hump and a slight linear increase of its amplitude detected during quiescence suggest that the accretion disk is not in a steady state.

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