The Library

Cataclysmic variables below the period gap : mass determinations of 14 eclipsing systems

Tools

Savoury, C. D. J., Littlefair, S. P., Dhillon, V. S., Marsh, T. R., Gänsicke, B. T. (Boris T.), Copperwheat, C. M., Kerry, P., Hickman, R. D. G. (Richard D. G.) and Parsons, S. G.. (2011) Cataclysmic variables below the period gap : mass determinations of 14 eclipsing systems. Monthly Notices of the Royal Astronomical Society, Vol.415 (No.3). pp. 2025-2041. ISSN 00358711

Preview

PDF
WRAP_Marsh_1103.2713v1.pdf - Accepted Version - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
Download (3813Kb)

Official URL: http://dx.doi.org/10.1111/j.1365-2966.2011.18707.x

Abstract

We present high-speed, three-colour photometry of the eclipsing cataclysmic variables CTCV J1300-3052, CTCV J2354-4700 and SDSS J115207.00+404947.8. These systems have orbital periods of 128.07, 94.39 and 97.52 minutes respectively, placing all three systems below the observed “period gap” for cataclysmic variables. For each system we determine the system parameters by fitting a parameterised model to the observed eclipse light curve by χ2 minimisation. We also present an updated analysis of all other eclipsing systems previously analysed by our group. The updated analysis utilises Markov Chain Monte Carlo techniques which enable us to arrive confidently at the best fits for each system with more robust determinations of our errors. A new bright spot model is also adopted, that allows better modelling of bright-spot dominated systems. In addition, we correct a bug in the old code which resulted in the white dwarf radius being underestimated, and consequently both the white dwarf and donor mass being overestimated. New donor masses are generally between 1 and 2σ of those originally published, with the exception of SDSS 1502 (−2.9σ, Mr = −0.012M⊙) and DV UMa (+6.1σ, Mr = +0.039M⊙). We note that the donor mass of SDSS 1501 has been revised upwards by 0.024M⊙ (+1.9σ). This system was previously identified as having evolved passed the minimum orbital period for cataclysmic variables, but the new mass determination suggests otherwise. Our new analysis confirms that SDSS 1035 and SDSS 1433 have evolved past the period minimum for cataclysmic variables, corroborating our earlier studies. We find that the radii of donor stars are oversized when compared to theoretical models, by approximately 10 percent. We show that this can be explained by invoking either enhanced angular momentum loss, or by taking into account the effects of star spots. We are unable to favour one cause over the other, as we lack enough precise mass determinations for systems with orbital periods between 100 and 130 minutes, where evolutionary tracks begin to diverge significantly. We also find a strong tendency towards high white dwarf masses within our sample, and no evidence for any He-core white dwarfs. The dominance of high mass white dwarfs implies that erosion of the white dwarf during the nova outburst must be negligible, or that not all of the mass accreted is ejected during nova cycles, resulting in the white dwarf growing in mass.

[error in script] [error in script]

Item Type:	Journal Article
Subjects:	Q Science > QB Astronomy
Divisions:	Faculty of Science > Physics
Library of Congress Subject Headings (LCSH):	Eclipsing binaries, Cataclysmic variable stars
Journal or Publication Title:	Monthly Notices of the Royal Astronomical Society
Publisher:	Wiley
ISSN:	00358711
Date:	August 2011
Volume:	Vol.415
Number:	No.3
Page Range:	pp. 2025-2041
Identification Number:	10.1111/j.1365-2966.2011.18707.x
Status:	Peer Reviewed
Publication Status:	Published
Access rights to Published version:	Restricted or Subscription Access
Funder:	Science and Technology Facilities Council (Great Britain) (STFC), Research Councils UK (RCUK)
Grant number:	ST/F002599/1 (STFC), ST/G003092/1 (STFC)
References:	Bergeron P., Wesemael F., Beauchamp A., 1995, PASP, 107, 1047 Chabrier G., Gallardo J., Baraffe I., 2007, A&A, 472, L17 Copperwheat C., Marsh T., Dhillon V., Littlefair S., Hickman R., G¨ansicke B., Southworth J., 2010, MNRAS, 402, 1824 D’Cruz N., Dorman B., Rood R., O’Connell R., 1996, ApJ, 446, 359 Dhillon V., et al 2007, MNRAS, 378, 825 Epelstain N., Yaron O., Kovetz A., Prialnik D., 2007, MNRAS, 374, 1449 Feline W., 2005, PhD thesis, The University of Sheffield Feline W., Dhillon V., Marsh T., Stevenson M., Watson C., Brinkworth C., 2004a, MNRAS, 347, 1173 Feline W., Dhillon V., Marsh T., Brinkworth C., 2004b, MNRAS, 355, 1 Ford E., 2006, ApJ, 642, 505 G¨ansicke B., Dillon M., Southworth J., Thornstensen J., Rodr´ıguez-Gil P., Aungwerojwit A., Marsh T., et al. 2009, MNRAS, 397, 2170 Gregory P., 2007, MNRAS, 381, 1607 Hamada T., Salpeter E., 1961, ApJ, 134, 683 Hellier C., 2001, Cataclysmic Variable Stars. Praxis Publishing Ltd, Chichester Horne K., Marsh T., Cheng F., Hubany I., Lanz T., 1994, ApJ, 426, 294 Kepler S., Kleinman S., Nitta A., Koester D., Castanheira B., Giovannini O., Althaus L., 2007, in Napiwotzki R., Burleigh M., eds, 15th European Workshop on White Dwarfs Vol. 372 of ASPCS, The white dwarf mass distribution. pp 35–40 Knigge C., 2006, MNRAS, 373, 484 Kolb U., 1993, A&A, 271, 149 Kolb U., Baraffe I., 1999, MNRAS, 309, 1034 Liebert J., Bergeron P., Holberg J., 2005, ApJS, 156, 47 Littlefair S., Dhillon V., Martn E., 2003, MNRAS, 340, 264 Littlefair S., Dhillon V., Marsh T., G¨ansicke B., 2006a, MNRAS, 371, 1435 Littlefair S., Dhillon V., Marsh T., G¨ansicke B., Southworth J., Watson C., 2006b, Sci, 314, 1578 Littlefair S., Dhillon V., Marsh T., G¨ansicke B., Baraffe I., Watson C., 2007, MNRAS, 381, 827 Littlefair S., Dhillon V., Marsh T., G¨ansicke B., Southworth J., Baraffe I., Watson C., Copperwheat C., 2008, MNRAS, 388, 1582 Paczynski B., 1981, Acta Astron., 31, 1 Panei J., Althaus L., Benvenuto O., 2000, A&A, 353, 970 Patterson J., 1998, PASP, 110, 1132 Patterson J., 2009, ArXiv e-prints Patterson J., Thornstensen J., Knigge C., 2008, PASP, 120, 510 Pickles A., 1998, PASP, 110, 863 Ritter H., 1976, MNRAS, 175, 279 Ritter H., 1985, A&A, 148, 207 Ritter H., Burkert A., 1986, A&A, 158, 161 Roberts G., Gelman A., Gilks W., 1997, Annual of Applied Probability, 7, 110 Robinsons E. L., 1976, ApJ, 203, 485 Sirotkin F. V., Kim W.-T., 2010, ApJ, 721, 1356 Smith D., Dhillon V., 1998, MNRAS, 301, 767 Smith J., et al. 2002, AJ, 123, 2121 Southworth J., Copperwheat C. M., G¨ansicke B. T., Pyrzas S., 2010, A&A, 510, A100+ Szkody P., et al. 2004, ApJ, 128, 1882 Szkody P., et al. 2005, ApJ, 129, 2386 Szkody P., et al. 2006, ApJ, 131, 973 Szkody P., et al. 2007, ApJ, 134, 185 Tappert C., Augusteijn T., Maza J., 2004, MNRAS, 354, 321 Townsley D., G¨ansicke B., 2009, ApJ, 693, 1007 Tulloch S., Rodr´ıguez-Gil P., Dhillon V., 2009, MNRAS, 397, L82 Warner B., 1973, MNRAS, 162, 189 Warner B., 1976, in IAU Symposium, Vol.73, Structure and Evolution of Close Binary Systems, ed. P. Eggleton, S. Mitton & J.Whelan, 85-+ Warner B., 1995, Cataclysmic Variable Stars. Cambridge University Press, Cambridge Willems B., Kolb U., Sandquist E., Taam R., Dubus G., 2005, ApJ, 635, 1263 Wood J., Irwin M., Pringle J., 1985, MNRAS, 214, 475 Wood J., Horne K., Berriman G., Wade R., O’Donoghue D., Warner B., 1986, MNRAS, 219, 629 Wood M., 1995, in Koester D., Werner K., eds, LNP Vol. 443, White Dwarfs. Springer-Verlag, Berlin. p.41 Yaron O., Prialnik D., Shara M., Kovetz A., 2005, ApJ, 623, 398 Zorotovic, M., Schriber. M.R., G¨ansicke., B.T., 2011, A&A, submitted
URI:	http://wrap.warwick.ac.uk/id/eprint/38500