2MASS J10274572+0629104: the very short period young M6 dwarf binary system identified in K2 data

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https://academic.oup.com/mnras/article/486/3/4144/5454774?searchresult=1

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https://doi.org/10.1093/mnras/stz1067
 http://hdl.handle.net/11603/24259

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UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)

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https://orcid.org/0000-0002-8090-3570

Date

2019-04-13

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journal articles
preprints
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Citation of Original Publication

R R Paudel, J E Gizis, A J Burgasser, C Hsu, 2MASS J10274572+0629104: the very short period young M6 dwarf binary system identified in K2 data, Monthly Notices of the Royal Astronomical Society, Volume 486, Issue 3, July 2019, Pages 4144–4148, https://doi.org/10.1093/mnras/stz1067

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This is a pre-copyedited, author-produced PDF of an article accepted for publication Monthly Notices of the Royal Astronomical Society following peer review. The version of record R R Paudel, J E Gizis, A J Burgasser, C Hsu, 2MASS J10274572+0629104: the very short period young M6 dwarf binary system identified in K2 data, Monthly Notices of the Royal Astronomical Society, Volume 486, Issue 3, July 2019, Pages 4144–4148, https://doi.org/10.1093/mnras/stz1067 is available online at: https://academic.oup.com/mnras/article/486/3/4144/5454774?searchresult=1

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Abstract

We report the identification of a very low mass new binary system 2MASS J10274572+0629104, based on Kepler K2 photometry and Gaia DR2 astrometry. The K2 light curve is consistent with a beat pattern of two periodic signals, and using Lomb-Scargle periodogram, we find two rotation periods of 0.2114±0.0002 day and 0.2199±0.0003 day. We conclude that these rotation periods arise from two stars with similar spectral types of M6, and have near equal luminosity. It is the first ultracool binary system to be identified based on beat patterns in the light curve. Near-infrared spectroscopy yields RV = -9.8±0.6 km s⁻¹, v sin i =21.5±1.1 km s⁻¹, Tₑᶠᶠ = 3110±40 K, and log g = 5.2±0.2. The motions are consistent with a young age, as are the rotation periods, but the source does not appear to be part of any known moving group. Furthermore, we detected three strong white light flares in the K2 light curve, with estimated total bolometric (UV/optical/IR) energies to be 2.8 × 10³³, 5.2 × 10³³ and 3.8 × 10³³ erg respectively