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An “Accretor-Propeller” Model of CH Cygni

Published online by Cambridge University Press:  12 April 2016

M. Mikolajewski  and
J. Mikolajewska
M. Mikolajewski
Affiliation:
Institute of Astronomy, Nicolaus Copernicus University, Chopina 12/18, PL–87100 Torun, Poland
J. Mikolajewska
Affiliation:
Institute of Astronomy, Nicolaus Copernicus University, Chopina 12/18, PL–87100 Torun, Poland

Extract

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The most spectacular episode in the history of CH Cyg was undoubtedly a sudden drop of brightness (by about 1 mag) during the last weak of July 1984, coinciding with the ejection of two collimated jets (Taylor et al. 1985) perpendicular to the line of sight (Solf 1987) and the orbital plane (Luud et al. 1986). Supercritical accretion cannot be responsible for the jet ejection mechanism, because the luminosity of the accreting component was always about 2 orders of magnitude lower than the Eddington limit (Mikolajewska et al. 1987). This mechanism is also inconsistent with the rapid drop of brightness coinciding with the ejection of material. Simultaneously, it is conspicuous that the increase of brightness to optical maximum was also rapid (∼1 mag from July to September 1981; e.g. Kaler et al. 1983).

Type
Session 3. Physics of Individual Objects
Information
International Astronomical Union Colloquium , Volume 103: The Symbiotic Phenomenon , 1988 , pp. 233 - 234
Copyright
Copyright © Kluwer 1988

References

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