HII 2407: an eclipsing binary revealed by K2 observations of the Pleiades
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The star HII 2407 is a member of the relatively young Pleiades star cluster and was previously discovered to be a single-lined spectroscopic binary. It is newly identified here within Kepler/K2 photometric time series data as an eclipsing binary system. Mutual fitting of the radial velocity and photometric data leads to an orbital solution and constraints on fundamental stellar parameters. While the primary has arrived on the main sequence, the secondary is still pre-main sequence and we compare our results for the M/M⊙ and R/R⊙ values with stellar evolutionary models. We also demonstrate that the system is likely to be tidally synchronized. Follow-up infrared spectroscopy is likely to reveal the lines of the secondary, allowing for dynamically measured masses and elevating the system to benchmark eclipsing binary status.
David , T J , Stauffer , J , Hillenbrand , L A , Cody , A M , Conroy , K , Stassun , K G , Pope , B , Aigrain , S , Gillen , E , Collier Cameron , A , Barrado , D , Rebull , L M , Isaacson , H , Marcy , G W , Zhang , C , Riddle , R L , Ziegler , C , Law , N M & Baranec , C 2015 , ' HII 2407: an eclipsing binary revealed by K2 observations of the Pleiades ' Astrophysical Journal , vol 814 , no. 1 . DOI: 10.1088/0004-637X/814/1/62
© 2015. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: http://dx.doi.org/10.1088/0004-637X/814/1/62
The material presented herein is based upon work supported in 2015 by the National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. T.J.D. gratefully acknowledges support from France Córdova through the Neugebauer Scholarship. This research was partially supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. Support for this work was provided by NASA via grant NNX15AV62G. C.B. acknowledges support from the Alfred P. Sloan Foundation. A.C.C. acknowledges support from STFC grant ST/M001296/1. Funding for WASP comes from consortium universities and from UKs Science and Technology Facilities Council.
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