Davis, P. J.; Kolb, U.; Willems, B. and Gänsicke, B. T.
|DOI (Digital Object Identifier) Link:||http://dx.doi.org/10.1111/j.1365-2966.2008.13675.x|
|Google Scholar:||Look up in Google Scholar|
We apply population synthesis techniques to calculate the present-day number of two types of white-dwarf main-sequence star (WDMS) binaries within the cataclysmic variable 2 to 3 h period gap. The first are post-common envelope binaries with secondary stars that have masses 0.17 ≤M2/M⊙≤ 0.36 gap-post common envelope binaries (gPCEBs), such that they will commence mass transfer within the period gap. The second type are systems that were cataclysmic variables (CVs) at some point in their past, but detached once they evolved down in orbital period to ≈3 h as a consequence of disrupted magnetic braking, and are crossing the period gap via gravitational radiation detached cataclysmic variables (dCVs). Full population synthesis calculations are performed where we either assume constant, global values of the common envelope ejection efficiency, αCE , or consider αCE as a function of secondary mass. Several forms of magnetic braking are also considered. We predict an excess of dCVs over gPCEBs within the period gap of ∼4 to ∼13 assuming αCE= 0.1–0.6 , and an initial mass ratio distribution of the form n(q) = 1 . This excess is revealed as a prominent peak at the location of the period gap in the orbital period distribution of the combined gPCEB and dCV population. We suggest that if such a feature is observed in the orbital period distribution of an observed sample of short orbital period WDMS binaries, this would strongly corroborate the disruption of magnetic braking.
|Item Type:||Journal Article|
|Keywords:||methods: statistical; binaries: close; stars: evolution; novae, cataclysmic variables|
|Academic Unit/Department:||Science > Physical Sciences|
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)
|Depositing User:||Colin Smith|
|Date Deposited:||14 Apr 2009 15:37|
|Last Modified:||05 Mar 2014 10:27|
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