Journal Article

Physical properties of IP Pegasi: an eclipsing dwarf nova with an unusually cool white dwarf

C. M. Copperwheat, T. R. Marsh, V. S. Dhillon, S. P. Littlefair, R. Hickman, B. T. Gänsicke and J. Southworth

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 402, issue 3, pages 1824-1840
Published in print March 2010 | ISSN: 0035-8711
Published online February 2010 | e-ISSN: 1365-2966 | DOI:
Physical properties of IP Pegasi: an eclipsing dwarf nova with an unusually cool white dwarf

More Like This

Show all results sharing this subject:

  • Astronomy and Astrophysics


Show Summary Details


We present high-speed photometric observations of the eclipsing dwarf nova IP Pegasi (IP Peg) taken with the triple-beam camera ULTRACAM mounted on the William Herschel Telescope. The primary eclipse in this system was observed twice in 2004, and then a further 16 times over a 3 week period in 2005. Our observations were simultaneous in the Sloan u′, g′ and r′ bands. By phase-folding and averaging our data, we make the first significant detection of the white dwarf ingress in this system and find the phase width φ of the white dwarf eclipse to be 0.0935 ± 0.0003, significantly higher than the previous best value of 0.0863 < φ < 0.0918. The mass ratio is found to be q=M2/M1= 0.48 ± 0.01, consistent with previous measurements, but we find the inclination to be , significantly higher than previously reported. We find the radius of the white dwarf to be 0.0063 ± 0.0003 R, implying a white dwarf mass of 1.16 ± 0.02 M. The donor mass is 0.55 ± 0.02 M. The white dwarf temperature is more difficult to determine, since the white dwarf is seen to vary significantly in flux, even between consecutive eclipses. This is seen particularly in the u′ band, and is probably the result of absorption by disc material. Our best estimate of the temperature is 10 000–15 000 K, which is much lower than would be expected for a cataclysmic variable star with this period, and implies a mean accretion rate of <5 × 10−11 M yr−1, more than 40 times lower than the expected rate.

Keywords: stars: dwarf novae; stars: individual: IP Pegasi; white dwarfs

Journal Article.  13736 words.  Illustrated.

Subjects: Astronomy and Astrophysics

Full text: subscription required

How to subscribe Recommend to my Librarian

Users without a subscription are not able to see the full content. Please, subscribe or login to access all content.