Bibcode
Green, M. J.; Hermes, J. J.; Marsh, T. R.; Steeghs, D. T. H.; Bell, Keaton J.; Littlefair, S. P.; Parsons, S. G.; Dennihy, E.; Fuchs, J. T.; Reding, J. S.; Kaiser, B. C.; Ashley, R. P.; Breedt, E.; Dhillon, V. S.; Gentile Fusillo, N. P.; Kerry, P.; Sahman, D. I.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society, Volume 477, Issue 4, p.5646-5656
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7
2018
Citations
20
Refereed citations
19
Description
We present the discovery of SDSS J135154.46-064309.0, a short-period
variable observed using 30-mincadence photometry in K2 Campaign 6.
Follow-up spectroscopy and high-speed photometry support a
classification as a new member of the rare class of ultracompact
accreting binaries known as AM CVn stars. The spectroscopic orbital
period of 15.65 ± 0.12 min makes this system the
fourth-shortest-period AM CVn known, and the second system of this type
to be discovered by the Kepler spacecraft. The K2 data show photometric
periods at 15.7306 ± 0.0003 min, 16.1121 ± 0.0004 min, and
664.82 ± 0.06 min, which we identify as the orbital period,
superhump period, and disc precession period, respectively. From the
superhump and orbital periods we estimate the binary mass ratio q =
M2/M1= 0.111 ± 0.005, though this method of
mass ratio determination may not be well calibrated for helium-dominated
binaries. This system is likely to be a bright foreground source of
gravitational waves in the frequency range detectable by Laser
Interferometer Space Antenna, and may be of use as a calibration source
if future studies are able to constrain the masses of its stellar
components.
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Binary Stars
The study of binary stars is essential to stellar astrophysics. A large number of stars form and evolve within binary systems. Therefore, their study is fundamental to understand stellar and galactic evolution. Particularly relevant is that binary systems are still the best source of precise stellar mass and radius measurements. Research lines
Pablo
Rodríguez Gil