A highly unequal-mass eclipsing M-dwarf binary in the WFCAM Transit Survey

Nefs, S. V.; Birkby, Jayne; Snellen, I. A. G.; Hodgkin, S. T.; Sipőcz, Brigitta; Kovács, G.; Mislis, D.; Pinfield, D. J.; Martín, E. L.

doi:10.1093/mnras/stt405

Cited by 40 publications

(31 citation statements)

References 108 publications

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“…Using different stellar models for the characterization of the primary star did not lead to significant changes in the mass-radius relation of either of the stars. (Ségransan et al 2003;Bouchy et al 2005;Pont et al 2005Pont et al , 2006Hebb et al 2006;Beatty et al 2007;Maxted et al 2007;Blake et al 2008;Fernandez et al 2009;Morales et al 2009;Vida et al 2009;Dimitrov & Kjurkchieva 2010;Parsons et al 2010Parsons et al , 2012Hartman et al 2011;Carter et al 2011;Irwin et al 2011;Pyrzas et al 2012;Nefs et al 2013;Tal-Or et al 2013;Gómez Maqueo Chew et al 2014;Zhou et al 2014) and spectroscopic characterized single low mass stars (gray triangles) (Mann et al 2015). The best fit to data from Mann et al (2015) is given by the green dashed line.…”

Section: Resultsmentioning

confidence: 99%

“…For these stars, stellar models also show systematic discrepancies in the observed mass-radius relations, but on a larger scale. Over 30 eclipsing very low-mass stars (VLMSs) with masses below 0.3 M e and radii known to better than 10% have been observed so far (e.g., Parsons et al 2012;Pyrzas et al 2012;Nefs et al 2013;Gómez Maqueo Chew et al 2014;Zhou et al 2014;Kraus et al 2015;David et al 2016). However, only eight have radii known to a precision better than 2%.…”

Section: Introductionmentioning

confidence: 99%

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An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

Eigmüller¹,

Eislöffel²,

Csizmadia³

et al. 2016

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Only a few well characterized very low-mass M dwarfs are known today. Our understanding of M dwarfs is vital as these are the most common stars in our solar neighborhood. We aim to characterize the properties of a rare F+dM stellar system for a better understanding of the low-mass end of the Hertzsprung-Russel diagram. We used photometric light curves and radial velocity follow-up measurements to study the binary. Spectroscopic analysis was used in combination with isochrone fitting to characterize the primary star. The primary star is an early F-type main-sequence star with a mass of (1.493 ± 0.073) M e and a radius of (1.474 ± 0.040) R e . The companion is an M dwarf with a mass of (0.188 ± 0.014) M e and a radius of (0.234 ± 0.009) R e . The orbital period is (1.35121±0.00001) days. The secondary star is among the lowest-mass M dwarfs known to date. The binary has not reached a 1:1 spin-orbit synchronization. This indicates a young main-sequence binary with an age below ∼250 Myr. The mass-radius relation of both components are in agreement with this finding.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

Eigmüller¹,

Eislöffel²,

Csizmadia³

et al. 2016

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“…We overplotted three transiting brown dwarfs with accurate masses (below 30 Jupiter masses) and radii (Corot-3 b; KELT-1 b; Kepler-39 b; Deleuil et al 2008;Siverd et al 2012;Bouchy et al 2011). We also overplotted very-low mass components of the eclipsing binaries listed in Table 3 of Tal-Or et al (2013) whose masses range from 0.08 to 0.2 M (Pont et al 2005a(Pont et al ,b, 2006Hebb et al 2006;Maxted et al 2007;Beatty et al 2007;Pyrzas et al 2009Pyrzas et al , 2012Parsons et al 2012b,c,a;Ofir et al 2012;Triaud et al 2013) and added the M-dwarf system from the WFCAM Transit Survey published by Nefs et al (2013). We can see that most low-mass and brown dwarf components of eclipsing systems plotted in Fig.…”

Section: Usco16m25 In the Realm Of Eclipsing Binariesmentioning

confidence: 99%

An eclipsing double-line spectroscopic binary at the stellar/substellar boundary in the Upper Scorpius OB association

Lodieu

Alonso

Hernández

et al. 2015

A&A

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Aims. We aim at constraining evolutionary models at low mass and young ages by identifying interesting transiting system members of the nearest OB association to the Sun, Upper Scorpius (USco), which has been targeted by the Kepler mission. Methods. We produced light curves for M-dwarf members of the USco region that has been surveyed during the second campaign of the Kepler K2 mission. We identified by eye a transiting system, USco J161630.68−251220.1 (=EPIC 203710387) with a combined spectral type of M5.25, whose photometric, astrometric, and spectroscopic properties makes it a member of USco. We conducted an extensive photometric and spectroscopic follow-up of this transiting system with a suite of telescopes and instruments to characterise the properties of each component of the system. Results. We calculated a transit duration of about 2.42 h that occurs every 2.88 days with a slight difference in transit depth and phase between the two components. We estimated a mass ratio of 0.922 ± 0.015 from the semi-amplitudes of the radial velocity curves for each component. We derived masses of 0.091 ± 0.005 M and 0.084 ± 0.004 M , radii of 0.388 ± 0.008 R and 0.380 ± 0.008 R , luminosities of log(L/L ) = −2.020 Conclusions. We present a complete photometric and radial velocity characterisation of the least massive double-line eclipsing binary system in the young USco association with two components close to the stellar/substellar limit. This system falls in a gap between the least massive eclipsing binaries in the low-mass and substellar regimes at young ages and represents an important addition to constraining evolutionary models at young ages.

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“…However, Irwin et al (2011) found that the combined radii of the two stars in the LSPM J1112+7626 system are inflated by 3.8%. Even with the discovery of additional systems, there are only a handful of M-M EBs known that can be used to test theoretical models (Irwin et al 2011;Birkby et al 2012;Nefs et al 2013;Zhou et al 2015;Dittmann et al 2017). …”

Section: Introductionmentioning

confidence: 99%

A Bright Short Period M-M Eclipsing Binary from the KELT Survey: Magnetic Activity and the Mass–Radius Relationship for M Dwarfs

Lubin

Rodriguez

Zhou

et al. 2017

ApJ

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We report the discovery of KELT J041621-620046, a moderately bright (J∼10.2) M dwarf eclipsing binary system at a distance of 39±3 pc. KELT J041621-620046 was first identified as an eclipsing binary using observations from the Kilodegree Extremely Little Telescope (KELT) survey. The system has a short orbital period of ∼1.11 days and consists of components with M 1 = 0.447 +0.034 R ⊙ and R 2 = 0.453 ± 0.017 R ⊙ . Full system and orbital properties were determined (to ∼10% error) by conducting an EBOP global modeling of the high precision photometric and spectroscopic observations obtained by the KELT Follow-up Network. Each star is larger by 17-28% and cooler by 4-10% than predicted by standard (non-magnetic) stellar models. Strong Hα emission indicates chromospheric activity in both stars. The observed radii and temperature discrepancies for both components are more consistent with those predicted by empirical relations that account for convective suppression due to magnetic activity.

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A highly unequal-mass eclipsing M-dwarf binary in the WFCAM Transit Survey

Cited by 40 publications

References 108 publications

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

An eclipsing double-line spectroscopic binary at the stellar/substellar boundary in the Upper Scorpius OB association

A Bright Short Period M-M Eclipsing Binary from the KELT Survey: Magnetic Activity and the Mass–Radius Relationship for M Dwarfs

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