Abstract
A series of high time resolution spectra reveal the rapidly flickering, nova-like variable CD -42° 14462 to be a binary with P =.206 days and each component near one solar mass. The implied model is very similar to that found for the U Gem stars and old novae: an unseen lower main sequence star is transferring material onto a white dwarf. An accretion disk about the degenerate star is detected in weak H emissions. The phase dependence of both the velocity and intensity of these emissions indicates a hot spot on the following side of the accretion disk. Simultaneous rapid photometry reveals the flickering is not modulated with the orbital period, suggesting the inclination is too low for an eclipse or occultation of the hot spot.
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© 1977 D. Reidel Publishing Company, Dordrecht, Holland
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Cowley, A.P., Crampton, D., Hesser, J.E. (1977). The Binary Nature of the Nova-Like Variable CD -42° 14462. In: Friedjung, M. (eds) Novae and Related Stars. Astrophysics and Space Science Library, vol 65. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-1217-1_8
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DOI: https://doi.org/10.1007/978-94-010-1217-1_8
Publisher Name: Springer, Dordrecht
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