The minimum period problem in cataclysmic variables

Abstract

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 $P_{min}\approx 77$ 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. Put your abstract here.

10 pages, Latex, 13 postscript figures, Accepted for publication in MNRAS

References in corpus (8)

• Brown Dwarfs and the Cataclysmic Variable Period Minimum
• AE Aquarii: how CVs descend from supersoft binaries
• 1RXS J232953.9+062814: A Dwarf Nova with a 64-minute Orbital Period and a Conspicuous Secondary Star
• On the late spectral types of cataclysmic variable secondaries
• Blunting the Spike: the CV Minimum Period
• An eclipse of the X-ray flux from the dwarf nova OY Carinae in quiescence
• Nova-induced mass transfer variations
• Gravitational Wave Emission by Cataclysmic Variables: numerical models of semi-detached binaries

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