Exploring the M-dwarf Luminosity–Temperature–Radius relationships using Gaia DR2

Morrell, Sam; Naylor, T.

doi:10.1093/mnras/stz2242

Cited by 50 publications

(37 citation statements)

References 96 publications

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“…On the other side, the inability of the isochrone to adequately fit the bottom end of the sequence is a known problem (see e.g. Bell et al 2012;Morrell & Naylor 2019), and its discussion is beyond the scope of the present study.…”

Section: Colour-magnitude Diagrammentioning

confidence: 93%

Gyrochronological dating of the stellar moving group Group X

Messina

Nardiello

Desidera

et al. 2022

A&A

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Context. Gyrochronology is one of the methods currently used to estimate the age of stellar open clusters. Hundreds of new clusters, associations, and moving groups unveiled by Gaia and complemented by accurate rotation period measurements provided by recent space missions such as Kepler and TESS are allowing us to significantly improve the reliability of this method. Aims. We use gyrochronology, that is, the calibrated age-mass-rotation relation valid for low-mass stars, to measure the age of the recently discovered moving group Group X. Methods. We extracted the light curves of all candidate members from the TESS full frame images and measured their rotation periods using different period search methods. Results. We measured the rotation period of 168 of a total of 218 stars and compared their period-colour distribution with those of two age-benchmark clusters, the Pleiades (125 Myr) and Praesepe (625 Myr), as well as with the recently characterised open cluster NGC 3532 (300 Myr). Conclusions. As result of our analysis, we derived a gyro age of 300 ± 60 Myr. We also applied as independent methods the fitting of the entire isochrone and of the three brightest candidate members individually with the most precise stellar parameters, deriving comparable values of 250 Myr and 290 Myr, respectively. Our dating of Group X allows us to definitively rule out the previously proposed connection with the nearby but much older Coma Berenices cluster.

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Section: Colour-magnitude Diagrammentioning

confidence: 93%

Gyrochronological dating of the stellar moving group Group X

Messina

Nardiello

Desidera

et al. 2022

A&A

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“…We estimated the radii of the M dwarfs using a semi-empirical mass-radius relationship for M dwarfs, based on a combination of a large dataset of M dwarf radius measurements (Morrell & Naylor 2019) and the mass-luminosity relation from Mann et al (2019). This semi-empirical mass-radius relationship will be presented in more detail in a future publication (Brown et al, in prep) and leads to more accurate radius predictions compared to theoretical massradius relationships, which tend to under-predict the radii of lowmass stars by 5-10 per cent (López-Morales & Ribas 2005;Parsons et al 2018).…”

Section: Dwarf Masses and Radiimentioning

confidence: 99%

“…The disadvantage of using the -band being the intrinsic faintness of low-mass stars at these wavelengths. Fortunately the sample of M dwarfs presented by Morrell & Naylor (2019) We used this relation to estimate the M dwarf contribution to the -band fluxes in all the non-magnetic systems. The excess -band flux was then determined to be from the white dwarf.…”

Section: White Dwarf Temperaturesmentioning

confidence: 99%

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Magnetic white dwarfs in post-common-envelope binaries

Parsons

Gänsicke

Schreiber

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Magnitude-limited samples have shown that 20-25 per cent of cataclysmic variables contain white dwarfs with magnetic fields of Mega Gauss strength, in stark contrast to the approximately 5 per cent of single white dwarfs with similar magnetic field strengths. Moreover, the lack of identifiable progenitor systems for magnetic cataclysmic variables leads to considerable challenges when trying to understand how these systems form and evolve. Here we present a sample of six magnetic white dwarfs in detached binaries with low-mass stellar companions where we have constrained the stellar and binary parameters including, for the first time, reliable mass estimates for these magnetic white dwarfs. We find that they are systematically more massive than non-magnetic white dwarfs in detached binaries. These magnetic white dwarfs generally have cooling ages of more than 1 Gyr and reside in systems that are very close to Roche-lobe filling. Our findings are more consistent with these systems being temporarily detached cataclysmic variables, rather than pre-cataclysmic binaries, but we cannot rule out the latter possibility. We find that these systems can display unusual asymmetric light curves that may offer a way to identify them in larger numbers in future. Seven new candidate magnetic white dwarf systems are also presented, three of which have asymmetric light curves. Finally, we note that several newly identified magnetic systems have archival spectra where there is no clear evidence of magnetism, meaning that these binaries have been previously missed. Nevertheless, there remains a clear lack of younger detached magnetic white dwarf systems.

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“…One area where significant effort has been made is EBs containing low-mass stars. There remains a "radius inflation" problem for stars below 1 M in EBs, where theoretical models underpredict the measured radii by up to 15% and overpredict their T eff s. It has been suggested that this is due to tidal effects causing a faster rotation and thus a stronger magnetic field [172][173][174], but this conflicts with the fact that it has also been seen in single stars [175][176][177], so there is no current consensus on the cause [178]. One way to investigate this is to study EBs containing low-mass stars, preferably with a range of mass, metallicity and rotational velocity.…”

Section: "Normal" Ebsmentioning

confidence: 99%

Space-Based Photometry of Binary Stars: From Voyager to TESS

Southworth

2021

Universe

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Binary stars are crucial laboratories for stellar physics, so have been photometric targets for space missions beginning with the very first orbiting telescope (OAO-2) launched in 1968. This review traces the binary stars observed and the scientific results obtained from the early days of ultraviolet missions (OAO-2, Voyager, ANS, IUE), through a period of diversification (Hipparcos, WIRE, MOST, BRITE), to the current era of large planetary transit surveys (CoRoT, Kepler, TESS). In this time observations have been obtained of detached, semi-detached and contact binaries containing dwarfs, sub-giants, giants, supergiants, white dwarfs, planets, neutron stars and accretion discs. Recent missions have found a huge variety of objects such as pulsating stars in eclipsing binaries, multi-eclipsers, heartbeat stars and binaries hosting transiting planets. Particular attention is paid to eclipsing binaries, because they are staggeringly useful, and to the NASA Transiting Exoplanet Survey Satellite (TESS) because its huge sky coverage enables a wide range of scientific investigations with unprecedented ease. These results are placed into context, future missions are discussed, and a list of important science goals is presented.

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Exploring the M-dwarf Luminosity–Temperature–Radius relationships using Gaia DR2

Cited by 50 publications

References 96 publications

Gyrochronological dating of the stellar moving group Group X

Gyrochronological dating of the stellar moving group Group X

Magnetic white dwarfs in post-common-envelope binaries

Space-Based Photometry of Binary Stars: From Voyager to TESS

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