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Title:
Fortnightly fluctuations in the O-C diagram of CS 1246
Authors:
Barlow, B. N.; Dunlap, B. H.; Clemens, J. C.; Reichart, D. E.; Ivarsen, K. M.; Lacluyze, A. P.; Haislip, J. B.; Nysewander, M. C.
Affiliation:
AA(Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA), AB(Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA), AC(Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA), AD(SKYNET, Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA), AE(SKYNET, Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA), AF(SKYNET, Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA), AG(SKYNET, Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA), AH(Alion Science & Technology, 1000 Park Forty Plaza, Durham, NC 27713, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 414, Issue 4, pp. 3434-3443. (MNRAS Homepage)
Publication Date:
07/2011
Origin:
WILEY
Astronomy Keywords:
stars: individual: CS 1246, stars: oscillations, subdwarfs
Abstract Copyright:
© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS
DOI:
10.1111/j.1365-2966.2011.18645.x
Bibliographic Code:
2011MNRAS.414.3434B

Abstract

Dominated by a single, large-amplitude pulsation mode, the rapidly pulsating hot subdwarf B star CS 1246 is a prime candidate for a long-term O-C diagram study. We collected nearly 400 h of photometry with the 0.41-m Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes over a time-span of 14 months to begin looking for secular variations in the pulse timings. Interestingly, the O-C diagram is dominated by a strong sinusoidal pattern with a period of 14.1 d and an amplitude of 10.7 light-seconds. Underneath this sine wave is a secular trend implying a decrease in the 371.7-s pulsational period of ?, which we attribute to the evolution of the star through the Hertzsprung-Russell diagram. The sinusoidal variation could be produced by the presence of a low-mass companion, with m sin i~= 0.12 M&sun;, orbiting the subdwarf B star at a distance of 20 R&sun;. An analysis of the combined light curve reveals the presence of a low-amplitude first harmonic to the main pulsation mode. Based on observations at the SOAR Telescope, a collaboration between CPNq-Brazil, NOAO, UNC and MSU, and on observations collected at the PROMPT array via SKYNET.
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