Revising the properties of low mass eclipsing binary stars using TESS light curves

Jennings, Zachary G.; Southworth, J.; Maxted, P. F. L.; Mancini, L.

doi:10.1093/mnras/stad519

Cited by 7 publications

(5 citation statements)

References 77 publications

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“…The WASP survey is one among several ground-based transit surveys that have started post-2000 that have successfully confirmed transiting exoplanets [83][84][85][86][87][88][89][90][91]. All of these surveys produce many "false positives" [92][93][94][95] and other teams have also produced some efforts to characterise "EBLM-like" systems from these surveys, often with similar aims to the EBLM project itself [96][97][98][99][100][101].…”

Section: The Wasp Projectmentioning

confidence: 99%

“…The evolution of main-sequence M dwarfs is negligible within the lifetime of the Universe, but an age constraint is nevertheless useful to rule out the possibility that the M dwarf is a pre-main sequence star that is contracting towards the main sequence. [11,17,26,[30][31][32][33][34]36,38,[96][97][98][99]101,. The data used to generate this figure are available in the Supplementary Materials, File S1.…”

Section: An Updated View Of M-dwarf Propertiesmentioning

confidence: 99%

See 1 more Smart Citation

The EBLM Project—From False Positives to Benchmark Stars and Circumbinary Exoplanets

Maxted,

Triaud,

Martin

2023

Universe

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The EBLM project aims to characterise very-low-mass stars that are companions to solar-type stars in eclipsing binaries. We describe the history and motivation for this project, the methodology we use to obtain the precise mass, radius, and effective temperature estimates for very-low-mass M dwarfs, and review the results of the EBLM study and those from related projects. We show that radius inflation in fully convective stars is a more subtle effect than what was previously thought based on less precise measurements, i.e., the mass–radius–effective temperature relations we observe for fully convective stars in single-line eclipsing binaries show reasonable agreement with the theoretical models, particularly if we account for the M-dwarf metallicity, as inferred from the analysis of the primary star spectrum.

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Section: The Wasp Projectmentioning

confidence: 99%

Section: An Updated View Of M-dwarf Propertiesmentioning

confidence: 99%

The EBLM Project—From False Positives to Benchmark Stars and Circumbinary Exoplanets

Maxted,

Triaud,

Martin

2023

Universe

Self Cite

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“…It has been theorised that due to a correlation between radius inflation and effective temperature anomalies, luminosities predicted by models for low-mass stars are accurate (Delfosse et al 2000;Torres & Ribas 2002;Ribas 2006;Torres et al 2006;Torres 2007). This coupling of inflated radius with cooler effective temperature and vice versa has been termed the 'constant luminosity hypothesis' (Jennings et al 2023). More recent measurements and derived relations suggest that radius-temperature balance is only accurate to a few % (Mann et al 2019).…”

Section: Testing the Constant Luminosity Hypothesismentioning

confidence: 99%

“…First observed in the 1970s (Hoxie 1970(Hoxie , 1973Lacy 1977), this finding has continued to be observed ever since (Popper 1997;Clausen et al 1999;Torres & Ribas 2002;Casagrande et al 2008;Torres et al 2010;Kraus et al 2011;Birkby et al 2012;Feiden & Chaboyer 2012;Nefs et al 2013;Spada et al 2013;Torres 2013;Chen et al 2014;Dittmann et al 2017;Kesseli et al 2018;Swayne et al 2021;Morales et al 2022;Jennings et al 2023), being termed the "radius inflation" problem. Along with claims of radius inflation are reports of effective temperatures that are too cool compared to stellar models, a trend clearly visible in the mass-effective temperature diagram displayed in Parsons et al (2018).…”

Section: Introductionmentioning

confidence: 95%

The EBLM project – VIII. First results for M-dwarf mass, radius, and effective temperature measurements using CHEOPS light curves

Swayne

Maxted

Triaud

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The accuracy of theoretical mass, radius and effective temperature values for M-dwarf stars is an active topic of debate. Differences between observed and theoretical values have raised the possibility that current theoretical stellar structure and evolution models are inaccurate towards the low-mass end of the main sequence. To explore this issue we use the CHEOPS satellite to obtain high-precision light curves of eclipsing binaries with low mass stellar companions. We use these light curves combined with the spectroscopic orbit for the solar-type companion to measure the mass, radius and effective temperature of the M-dwarf star. Here we present the analysis of three eclipsing binaries. We use the pycheops data analysis software to fit the observed transit and eclipse events of each system. Two of our systems were also observed by the TESS satellite– we similarly analyse these light curves for comparison. We find consistent results between CHEOPS and TESS, presenting three stellar radii and two stellar effective temperature values of low-mass stellar objects. These initial results from our on-going observing programme with CHEOPS show that we can expect to have ∼24 new mass, radius and effective temperature measurements for very low mass stars within the next few years.

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“…Many interesting eclipsing systems have been manually investigated in depth to great effect, providing physical insights on a case-by-case basis (e.g. Schmid & Aerts 2016;Johnston et al 2019a;Jennings et al 2023;Pavlovski et al 2023;Rosu et al 2023, to name just a few). It is through these kinds of studies that we can calibrate in detail our models of stars, for example with regards to the discrepancy between the dynamical and evolutionary masses of intermediate-to high-mass stars (e.g.…”

Section: Introductionmentioning

confidence: 99%

Automated eccentricity measurement from raw eclipsing binary light curves with intrinsic variability

IJspeert,

Tkachenko,

Johnston

et al. 2024

A&A

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Eclipsing binary systems provide the opportunity to measure the fundamental parameters of their component stars in a stellar-model-independent way. This makes them ideal candidates for testing and calibrating theories of stellar structure and (tidal) evolution. Large photometric (space) surveys provide a wealth of data for both the discovery and the analysis of these systems. Even without spectroscopic follow-up there is often enough information in their photometric time series to warrant analysis, especially if there is an added value present in the form of intrinsic variability, such as pulsations. Our goal is to implement and validate a framework for the homogeneous analysis of large numbers of eclipsing binary light curves, such as the numerous high-duty-cycle observations from space missions like TESS. The aim of this framework is to be quick and simple to run and to limit the user's time investment when obtaining, amongst other parameters, orbital eccentricities. We developed a new and fully automated methodology for the analysis of eclipsing binary light curves with or without additional intrinsic variability. Our method includes a fast iterative pre-whitening procedure that results in a list of extracted sinusoids that is broadly applicable for purposes other than eclipses. After eclipses are identified and measured, orbital and stellar parameters are measured under the assumption of spherical stars of uniform brightness. We tested our methodology in two settings: a set of synthetic light curves with known input and the catalogue of Kepler eclipsing binaries. The synthetic tests show that we can reliably recover the frequencies and amplitudes of the sinusoids included in the signal as well as the input binary parameters, albeit to varying degrees of accuracy. Recovery of the tangential component of eccentricity is the most accurate and precise. Kepler results confirm a robust determination of orbital periods, with 80.5<!PCT!> of periods matching the catalogued ones. We present the eccentricities for this analysis and show that they broadly follow the theoretically expected pattern as a function of the orbital period. Our analysis methodology is shown to be capable of analysing large numbers of eclipsing binary light curves with no user intervention, and in doing so provide a basis for a further in-depth analysis of systems of particular interest as well as for statistical analysis at the sample level. Furthermore, the computational performance of the frequency analysis, extracting hundreds of sinusoids from Kepler light curves in a few hours, demonstrates its value as a tool for a field like asteroseismology.

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Revising the properties of low mass eclipsing binary stars using TESS light curves

Cited by 7 publications

References 77 publications

The EBLM Project—From False Positives to Benchmark Stars and Circumbinary Exoplanets

The EBLM Project—From False Positives to Benchmark Stars and Circumbinary Exoplanets

The EBLM project – VIII. First results for M-dwarf mass, radius, and effective temperature measurements using CHEOPS light curves

Automated eccentricity measurement from raw eclipsing binary light curves with intrinsic variability

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