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Five Dwarf Novae with Orbital Periods Below Two Hours

Autor: Thorstensen, J. R., Fenton, W. H.

We give mean spectra and report orbital periods Porb based on radial velocities taken near minimum light for five dwarf novae, all of which prove to have Porb less than 2 hr. The stars and their periods are KX Aql, 0.06035(3) d; FT Cam, 0.07492(8) d;

Externí odkaz: http://arxiv.org/abs/astro-ph/0209172

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QZ Serpentis: A Dwarf Nova with a 2-Hour Orbital Period and an Anomalously Hot, Bright Secondary Star

Autor: Thorstensen, J. R., Fenton, W. H., Patterson, J. O., Kemp, J., Halpern, J., Baraffe, I.

We present spectroscopy and time-series photometry of the dwarf nova QZ Ser. The spectrum shows a rich absorption line spectrum of type K4 +- 2. K-type secondary stars are generally seen in dwarf novae with orbital periods P-orb around 6 h, but in QZ

Externí odkaz: http://arxiv.org/abs/astro-ph/0206435

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The cataclysmic variable CW 1045+525: a secondary-dominated dwarf nova?

Autor: Tappert, C., Thorstensen, J. R., Fenton, W. H., Bennert, N., Schmidtobreick, L., Bianchini, A.

We present spectroscopic and photometric observations of the cataclysmic variable CW 1045+525. Both the optical spectrum and the photometric lightcurve show a strong contribution of a K5V - M0V secondary. We derive an orbital period P_orb = 0.271278(

Externí odkaz: http://arxiv.org/abs/astro-ph/0110406

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Heavy Element Diffusion in Metal Poor Stars

Autor: Chaboyer, Brian, Fenton, W. H., Nelan, Jenica E., Patnaude, D. J., Simon, Francesca E.

Publikováno v: Astrophys.J.562:521-527,2001

Stellar evolution models which include the effect of helium and heavy element diffusion have been calculated for initial iron abundances of [Fe/H] = -2.3, -2.1, -1.9 and -1.7. These models were calculated for a large variety of masses and three separ

Externí odkaz: http://arxiv.org/abs/astro-ph/0108119

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