Journal Article

Whole Earth Telescope observations of the subdwarf B star KPD 1930+2752: a rich, short-period pulsator in a close binary

M. D. Reed, S. L. Harms, S. Poindexter, A.-Y. Zhou, J. R. Eggen, M. A. Morris, A. C. Quint, S. McDaniel, A. Baran, N. Dolez, S. D. Kawaler, D. W. Kurtz, P. Moskalik, R. Riddle, S. Zola, R. H. Østensen, J.-E. Solheim, S. O. Kepler, A. F. M. Costa, J. L. Provencal, F. Mullally, D. W. Winget, M. Vuckovic, R. Crowe, D. Terry, R. Avila, B. Berkey, S. Stewart, J. Bodnarik, D. Bolton, P.-M. Binder, K. Sekiguchi, D. J. Sullivan, S.-L. Kim, W.-P. Chen, C.-W. Chen, H.-C. Lin, X.-J. Jian, H. Wu, J.-P. Gou, Z. Liu, E. Leibowitz, Y. Lipkin, C. Akan, O. Cakirli, R. Janulis, R. Pretorius, W. Ogloza, G. Stachowski, M. Paparo, R. Szabo, Z. Csubry, D. Zsuffa, R. Silvotti, S. Marinoni, I. Bruni, G. Vauclair, M. Chevreton, J. M. Matthews, C. Cameron and H. Pablo

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 412, issue 1, pages 371-390
Published in print March 2011 | ISSN: 0035-8711
Published online March 2011 | e-ISSN: 1365-2966 | DOI:
Whole Earth Telescope observations of the subdwarf B star KPD 1930+2752: a rich, short-period pulsator in a close binary

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KPD 1930+2752 is a short-period pulsating subdwarf B (sdB) star. It is also an ellipsoidal variable with a known binary period of 2.3 h. The companion is most likely a white dwarf and the total mass of the system is close to the Chandresekhar limit. In this paper, we report the results of Whole Earth Telescope (WET) photometric observations during 2003 and a smaller multisite campaign of 2002. From 355 h of WET data, we detect 68 pulsation frequencies and suggest an additional 13 frequencies within a crowded and complex temporal spectrum between 3065 and 6343 μHz (periods between 326 and 157 s). We examine pulsation properties including phase and amplitude stability in an attempt to understand the nature of the pulsation mechanism. We examine a stochastic mechanism by comparing amplitude variations with simulated stochastic data. We also use the binary nature of KPD 1930+2752 for identifying pulsation modes via multiplet structure and a tidally induced pulsation geometry. Our results indicate a complicated pulsation structure that includes short-period (≈16 h) amplitude variability, rotationally split modes, tidally induced modes and some pulsations which are geometrically limited on the sdB star.

Keywords: binaries: close; stars: general; stars: oscillations; subdwarfs; oscillations: individual: KPD 1930+2752

Journal Article.  9342 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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