Barker, J. and Kolb, U.
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We investigate if consequential angular momentum losses (CAML) or an intrinsic deformation of the donor star in CVs could increase the CV bounce period from the canonical theoretical value ~65 min to the observed value min, and if a variation of these effects in a CV population could wash out the theoretically predicted accumulation of systems near the minimum period (the period spike). We are able to construct suitably mixed CV model populations that a statisticial test cannot rule out as the parent population of the observed CV sample. However, the goodness of fit is never convincing, and always slightly worse than for a simple, flat period distribution. Generally, the goodness of fit is much improved if all CVs are assumed to form at long orbital periods. The weighting suggested by King, Schenker & Hameury (2002) does not constitute an improvment if a realistically shaped input period distribution is used.
|Item Type:||Conference Item|
|Extra Information:||The Physics of Cataclysmic Variables and Related Objects, ASP Conference Proceedings, Vol. 261. Edited by B. T. Gänsicke, K. Beuermann, and K. Reinsch. ISBN: 1-58381-101-X. San Francisco: Astronomical Society of the Pacific, 2002, p. 271.
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|Keywords:||binaries; stars; evolution; mass-loss; novae; cataclysmic variables|
|Academic Unit/Department:||Science > Physical Sciences|
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Users 6041 not found.|
|Date Deposited:||22 Dec 2006|
|Last Modified:||24 Nov 2014 12:00|
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