CoRoT 101186644: A transiting low-mass dense M-dwarf on an eccentric 20.7-day period orbit around a late F-star

Tal-Or, L.; Mazeh, T.; Alonso, R.; Bouchy, F.; Cabrera, J.; Deeg, H. J.; Deleuil, M.; Faigler, S.; Fridlund, M.; Hébrard, G.; Moutou, C.; Santerne, A.; Tingley, B.

doi:10.1051/0004-6361/201220862

Cited by 25 publications

(15 citation statements)

References 79 publications

(67 reference statements)

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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%

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%

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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“…Grey circles indicate the mass and radius of red dwarfs in other PCEB binaries (Parsons et al 2010b(Parsons et al , 2012b(Parsons et al ,c, 2016. Grey squares indicate the mass and radius of single red dwarfs or red dwarfs with a main-sequence companion from Beatty et al 2007;López-Morales 2007;Nefs et al 2013;Tal-Or et al 2013;Zhou et al 2014. Table 2.…”

Section: Mass Radius and Temperaturementioning

confidence: 99%

PTF1 J085713+331843, a new post-common-envelope binary in the orbital period gap of cataclysmic variables

Roestel

Groot

Levitan

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We report the discovery and analysis of PTF1 J085713+331843, a new eclipsing post common-envelope detached white-dwarf red-dwarf binary with a 2.5h orbital period discovered by the Palomar Transient Factory. ULTRACAM multicolour photometry over multiple orbital periods reveals a light curve with a deep flat-bottomed primary eclipse and a strong reflection effect. Phase-resolved spectroscopy shows broad Balmer absorption lines from the DA white dwarf and phase-dependent Balmer emission lines originating on the irradiated side of the red dwarf. The temperature of the DA white dwarf is T WD = 25700±400 K and the spectral type of the red dwarf is M3-5. A combined modelling of the light curve and the radial velocity variations results in a white dwarf mass of M WD = 0.61 +0.18 −0.17 M and radius of R WD = 0.0175 +0.0012 −0.0011 R , and a red dwarf mass and radius of M RD = 0.19 +0.10 −0.08 M and R RD = 0.24 +0.04 −0.04 R . The system is either a detached cataclysmic variable or has emerged like from the common envelope phase at nearly its current orbital period. In ∼70 Myr, this system will become a cataclysmic variable in the period gap.

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“…The center-of-eclipse times for the 49 primary and 50 secondary eclipses were measured in two ways: (i) by using the best-fit model eclipse profile (described in Section 3) as a template and sliding it to best match the individual eclipses; and (ii) using the technique described in Steffen et al (2011) and Welsh et al (2012), which uses a template created from a polynomial fit to the folded eclipse profile. The results were very comparable, so we adopt the former method because it should be less-sensitive to starspot-induced deviations in the mean eclipse profile.…”

Section: The Kepler Light Curvesmentioning

confidence: 99%

“…The uncertainties listed are from the data calibration, but when used in the fitting process the uncertainties were boosted by a factor of 1.6 to achieve a reduced 2 c near 1.0. Several independent spectral analyses were carried out using the higher signal-to-noise HET spectra, including an Stellar Parameter Classification (SPC) analysis (Buchhave et al 2012), an analysis similar to the one for KOI-126 ), a MOOG-based analysis, and by fitting a theoretical template to the spectrum (Tal-Or et al 2013). Each gave similar results, with the best fit T eff ranging from 5480 to 5620 K, and metallicity [m H] ranging from −0.10 to +0.09.…”

Section: The Kepler Light Curvesmentioning

confidence: 99%

KEPLER 453 b—THE 10thKEPLERTRANSITING CIRCUMBINARY PLANET

Welsh

Orosz

Short

et al. 2015

ApJ

158

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We present the discovery of Kepler-453 b, a 6.2 R Å planet in a low-eccentricity, 240.5 day orbit about an eclipsing binary. The binary itself consists of a 0.94 and 0.195 M ☉ pair of stars with an orbital period of 27.32 days. The plane of the planetʼs orbit is rapidly precessing, and its inclination only becomes sufficiently aligned with the primary star in the latter portion of the Kepler data. Thus three transits are present in the second half of the light curve, but none of the three conjunctions that occurred during the first half of the light curve produced observable transits. The precession period is ∼103 years, and during that cycle, transits are visible only ∼8.9% of the time. This has the important implication that for every system like Kepler-453 that we detect, there are ∼11.5 circumbinary systems that exist but are not currently exhibiting transits. The planetʼs mass is too small to noticeably perturb the binary, and consequently its mass is not measurable with these data; however, our photodynamical model places a 1σ upper limit of M 16 Å . With a period 8.8 times that of the binary, the planet is well outside the dynamical instability zone. It does, however, lie within the habitable zone of the binary, making it the third of 10 Kepler circumbinary planets to do so.

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CoRoT 101186644: A transiting low-mass dense M-dwarf on an eccentric 20.7-day period orbit around a late F-star

Cited by 25 publications

References 79 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

PTF1 J085713+331843, a new post-common-envelope binary in the orbital period gap of cataclysmic variables

KEPLER 453 b—THE 10thKEPLERTRANSITING CIRCUMBINARY PLANET

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