期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 408, 期 1, 页码 L51-L55出版社
OXFORD UNIV PRESS
DOI: 10.1111/j.1745-3933.2010.00926.x
关键词
binaries: close; binaries: eclipsing; stars: individual: 2M1938+4603; subdwarfs; stars: variables: general
资金
- NASA's Science Mission Directorate
- European Research Council [227224]
- Research Council of K. U. Leuven [GOA/2008/04]
- European Research Council (ERC) [227224] Funding Source: European Research Council (ERC)
- Science and Technology Facilities Council [ST/F002599/1] Funding Source: researchfish
- STFC [ST/F002599/1] Funding Source: UKRI
2M1938+4603 (KIC 9472174) displays a spectacular light curve dominated by a strong reflection effect and rather shallow, grazing eclipses. The orbital period is 0.126 d, the second longest period yet found for an eclipsing sdB+dM, but still close to the minimum 0.1-d period among such systems. The phase-folded Kepler light curve was used to detrend the orbital effects from the data set. The amplitude spectrum of the residual light curve reveals a rich collection of pulsation peaks spanning frequencies from similar to 50 to 4500 mu Hz. The presence of a complex pulsation spectrum in both the p- and g-mode regions has never before been reported in a compact pulsator. Eclipsing sdB+dM stars are very rare, with only seven systems known and only one with a pulsating primary. Pulsating stars in eclipsing binaries are especially important since they permit masses derived from seismological model fits to be cross-checked with orbital mass constraints. We present a first analysis of this star based on the Kepler 9.7-d commissioning light curve and extensive ground-based photometry and spectroscopy that allow us to set useful bounds on the system parameters. We derive a radial-velocity amplitude K-1 = 65.7 +/- 0.6 km s(-1), inclination angle i = 69 degrees.45 +/- 0 degrees.20, and find that the masses of the components are M-1 = 0.48 +/- 0.03 M-circle dot and M-2 = 0.12 +/- 0.01 M-circle dot
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