Photometric Study of Fourteen Low-mass Binaries<sup>∗</sup>

Korda, David; Zasche, P.; Wolf, M.; Kučáková, H.; Hoňková, K.; Vraštil, J.

doi:10.3847/1538-3881/aa7138

Cited by 6 publications

(5 citation statements)

References 39 publications

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“…This effect was further studied by a light-curve solution. The observable difference in mid-eclipse times of spotted components was also outlined recently by Korda et al (2017).…”

Section: O-c Diagramsupporting

confidence: 61%

“…Barros et al (2013) showed that observed transit time variations in the hot-Jupiter WASP-10b system are also due to spot occultation features. Moreover, Korda et al (2017) tested the spot variability on the light curve of low-mass binaries and found a difference in mid-eclipse times of about 95 s. Recently, Zaire et al (2022) announced, that the well-known eclipsing binary system V471 Tau has the magnetically active K2 dwarf component, which might be responsible for driving the eclipse timing variations with predicted ∼ 35 yr activity cycle.…”

Section: Introductionmentioning

confidence: 99%

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A photometric study of V608 Cam: apparent period changes as a result of surface activity

Šebek¹,

Walter²,

Wolf³

2022

Preprint

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The VRI light curves were measured for the low-mass eclipsing binary V608 Cam as a part of our long-term observational project for studying of eclipsing binaries with a short orbital period. The Tess light curve solution in Phoebe results to the detached configuration, where the temperature of primary component was fixed to T 1 = 5 300 K according to Gaia results, which gives us T 2 = 4 110±50 K for the secondary. The spectral type of the primary component was derived to be K0 and the photometric mass ratio was estimated q = 0.92 ± 0.07. Characteristics and temporal variation of the cold region on the surface of the secondary component were estimated and are attributed to apparent period changes of this eclipsing binary with a cycle of about 2.4 yr.

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“…This effect was further studied by a light-curve solution. The observable difference in mid-eclipse times of spotted components was also outlined recently by Korda et al (2017).…”

Section: O-c Diagramsupporting

confidence: 61%

Section: Introductionmentioning

confidence: 99%

A photometric study of V608 Cam: apparent period changes as a result of surface activity

Šebek¹,

Walter²,

Wolf³

2022

Preprint

Self Cite

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“…Such metallicity independence of the massradius relation for low-mass stars is also frequently found in evolutionary models (see, e.g., Fig. 3 The reasons for the intrinsic spread in the observed massradius relation and the comparison to theoretical models have been and are still being investigated elsewhere (e.g., Feiden & Chaboyer 2012;Korda et al 2017;Tognelli et al 2018;Parsons et al 2018). As pointed out by Parsons et al (2018), this spread sets a lower limit on the error bars for the masses obtained with this method.…”

Section: Masses (M M−r )supporting

confidence: 57%

The CARMENES search for exoplanets around M dwarfs: Different roads to radii and masses of the target stars

Schweitzer,

Passegger,

Cifuentes

et al. 2019

Preprint

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Aims. We determine the radii and masses of 293 nearby, bright M dwarfs of the CARMENES survey. This is the first time that such a large and homogeneous high-resolution (R > 80, 000) spectroscopic survey has been used to derive these fundamental stellar parameters. Methods. We derived the radii using Stefan-Boltzmann's law. We obtained the required effective temperatures T eff from a spectral analysis and we obtained the required luminosities L from integrated broadband photometry together with the Gaia DR2 parallaxes. The mass was then determined using a mass-radius relation that we derived from eclipsing binaries known in the literature. We compared this method with three other methods: (1) We calculated the mass from the radius and the surface gravity log g, which was obtained from the same spectral analysis as T eff . (2) We used a widely used infrared mass-magnitude relation. (3) We used a Bayesian approach to infer stellar parameters from the comparison of the absolute magnitudes and colors of our targets with evolutionary models. Results. Between spectral types M0 V and M7 V our radii cover the range 0.1 R < R < 0.6 R with an error of 2-3% and our masses cover 0.09 M < M < 0.6 M with an error of 3-5%. We find good agreement between the masses determined with these different methods for most of our targets. Only the masses of very young objects show discrepancies. This can be well explained with the assumptions that we used for our methods.

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“…The reasons for the intrinsic spread in the observed mass-radius relation and the comparison to theoretical models have been and are still being investigated elsewhere (e.g., Feiden & Chaboyer 2012;Korda et al 2017;Tognelli et al 2018;Parsons et al 2018). As pointed out by Parsons et al (2018), this spread sets a lower limit on the error bars for the masses obtained with this method.…”

Section: Masses (M M−r )mentioning

confidence: 99%

The CARMENES search for exoplanets around M dwarfs

Schweitzer

Passegger

Cifuentes

et al. 2019

A&A

181

177

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Aims. We determine the radii and masses of 293 nearby, bright M dwarfs of the CARMENES survey. This is the first time that such a large and homogeneous high-resolution (R > 80 000) spectroscopic survey has been used to derive these fundamental stellar parameters. Methods. We derived the radii using Stefan-Boltzmann's law. We obtained the required effective temperatures T eff from a spectral analysis and we obtained the required luminosities L from integrated broadband photometry together with the Gaia DR2 parallaxes. The mass was then determined using a mass-radius relation that we derived from eclipsing binaries known in the literature. We compared this method with three other methods: (1) We calculated the mass from the radius and the surface gravity log g, which was obtained from the same spectral analysis as T eff . (2) We used a widely used infrared mass-magnitude relation. (3) We used a Bayesian approach to infer stellar parameters from the comparison of the absolute magnitudes and colors of our targets with evolutionary models. Results. Between spectral types M0 V and M7 V our radii cover the range 0.1 R < R < 0.6 R with an error of 2-3% and our masses cover 0.09 M < M < 0.6 M with an error of 3-5%. We find good agreement between the masses determined with these different methods for most of our targets. Only the masses of very young objects show discrepancies. This can be well explained with the assumptions that we used for our methods.Article published by EDP Sciences A68, page 1 of 16 A&A 625, A68 (2019)

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Photometric Study of Fourteen Low-mass Binaries^∗

Cited by 6 publications

References 39 publications

A photometric study of V608 Cam: apparent period changes as a result of surface activity

A photometric study of V608 Cam: apparent period changes as a result of surface activity

The CARMENES search for exoplanets around M dwarfs: Different roads to radii and masses of the target stars

The CARMENES search for exoplanets around M dwarfs

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Photometric Study of Fourteen Low-mass Binaries∗

Cited by 6 publications

References 39 publications

A photometric study of V608 Cam: apparent period changes as a result of surface activity

A photometric study of V608 Cam: apparent period changes as a result of surface activity

The CARMENES search for exoplanets around M dwarfs: Different roads to radii and masses of the target stars

The CARMENES search for exoplanets around M dwarfs

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Photometric Study of Fourteen Low-mass Binaries^∗