Empirical Relations for the Accurate Estimation of Stellar Masses and Radii

Moya, A.; Zuccarino, Federico; Chaplin, W. J.; Davies, G. R.

doi:10.3847/1538-4365/aacdae

Cited by 32 publications

(77 citation statements)

References 55 publications

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“…The PDMF weighting strongly decreases with increasing mass following a multi-component power law (Kroupa 2002). A mean effective temperature (T eff ) is associated to each spectral type, and the corresponding main sequence mass is then computed from the mass -T eff relation of Moya et al (2018):…”

Section: The Pdmf-corrected Sb1 Fraction and Its Metallicity Dependencementioning

confidence: 99%

“…This empirical relation is accurate to better than 10% and is based on 125 stars among which 41% are eclipsing binaries, whereas 57% and 2% of the masses are derived from asteroseismic and interferometric observations, respectively. Moya et al (2018) investigated numerous other functional relations (e.g. stellar mass as a function of T eff and surface gravity) and, among those, some have better regression coefficients than the one we selected, which is nevertheless largely sufficient for our purpose.…”

Section: The Pdmf-corrected Sb1 Fraction and Its Metallicity Dependencementioning

confidence: 99%

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TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

Merle

Swaelmen

Eck

et al. 2020

A&A

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Context. Multiple stellar systems play a fundamental role in the formation and evolution of stellar populations in galaxies. Recent and ongoing large ground-based multi-object spectroscopic surveys significantly increase the sample of spectroscopic binaries (SBs) allowing analyses of their statistical properties. Aims. We investigate the repeated spectral observations of the Gaia-ESO Survey internal data release 5 (GES iDR5) to identify and characterise SBs with one visible component (SB1s) in fields covering mainly the discs, the bulge, the CoRot fields, and some stellar clusters and associations. Methods. A statistical χ 2 -test is performed on spectra of the iDR5 subsample of approximately 43 500 stars characterised by at least two observations and a signal-to-noise ratio larger than three. In the GES iDR5, most stars have four observations generally split into two epochs. A careful estimation of the radial velocity (RV) uncertainties is performed. Our sample of RV variables is cleaned from contamination by pulsation-and/or convection-induced variables using Gaia DR2 parallaxes and photometry. Monte-Carlo simulations using the SB9 catalogue of spectroscopic orbits allow to estimate our detection efficiency and to correct the SB1 rate to evaluate the GES SB1 binary fraction and its relation to effective temperature and metallicity. Results. We find 641 (resp., 803) FGK SB1 candidates at the 5σ (resp., 3σ) level. The maximum RV differences range from 2.2 km s −1 at the 5σ confidence level (1.6 km s −1 at 3σ) to 133 km s −1 (in both cases). Among them a quarter of the primaries are giant stars and can be located as far as 10 kpc. The orbital-period distribution is estimated from the RV standard-deviation distribution and reveals that the detected SB1s probe binaries with log P[d] 4. We show that SB1s with dwarf primaries tend to have shorter orbital periods than SB1s with giant primaries. This is consistent with binary interactions removing shorter period systems as the primary ascends the red giant branch. For two systems, tentative orbital solutions with periods of 4 and 6 d are provided. After correcting for detection efficiency, selection biases, and the present-day mass function, we estimate the global GES SB1 fraction to be in the range 7-14% with a typical uncertainty of 4%. A small increase of the SB1 frequency is observed from K-towards F-type stars, in agreement with previous studies. The GES SB1 frequency decreases with metallicity at a rate of (−9 ± 3)% dex −1 in the metallicity range −2.7 ≤[Fe/H]≤ +0.6. This anticorrelation is obtained with a confidence level higher than 93% on a homogeneous sample covering spectral types FGK and a large range of metallicities. When the present-day mass function is accounted for, this rate turns to (−4 ± 2)% dex −1 with a confidence level higher than 88%. In addition we provide the variation of the SB1 fraction with metallicity separately for F, G, and K spectral types, as well as for dwarf and giant primaries.

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Section: The Pdmf-corrected Sb1 Fraction and Its Metallicity Dependencementioning

confidence: 99%

Section: The Pdmf-corrected Sb1 Fraction and Its Metallicity Dependencementioning

confidence: 99%

TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

Merle

Swaelmen

Eck

et al. 2020

A&A

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“…It is thus extensively used as a reference object for empirical mass and radius calibrations (e.g. Torres et al 2010;Eker et al 2015;Moya et al 2018). A number of theoretical studies attempted to explain the inflated radii of the components of YY Gem by developing different versions of non-conventional stellar interior structure models which incorporated effects of magnetic field and surface inhomogeneities (Feiden & Chaboyer 2013;MacDonald & Mullan 2014, 2017aJackson & Jeffries 2014).…”

Section: Introductionmentioning

confidence: 99%

Magnetic Field of the Eclipsing M-dwarf Binary YY Gem

Kochukhov

Shulyak

2019

ApJ

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YY Gem is a short-period eclipsing binary system containing two nearly identical, rapidly rotating, very active early-M dwarfs. This binary represents an important benchmark system for calibrating empirical relations between fundamental properties of low-mass stars and for testing theories of interior structure and evolution of these objects. Both components of YY Gem exhibit inflated radii, which has been attributed to poorly understood magnetic activity effects. Despite a long history of magnetic activity studies of this system no direct magnetic field measurements have been made for it. Here we present a comprehensive characterisation of the surface magnetic field in both components of YY Gem. We reconstructed the global field topologies with the help of a tomographic inversion technique applied to high-resolution spectropolarimetric data. This analysis revealed moderately complex global fields with a typical strength of 200-300 G and anti-aligned dipolar components. A complementary Zeeman intensification analysis of the disentangled intensity spectra showed that the total mean field strength reaches 3.2-3.4 kG in both components of YY Gem. We used these results together with other recent magnetic field measurements of M dwarfs to investigate the relation between the global and small-scale fields in these stars. We also assessed predictions of competing magnetoconvection interior structure models developed for YY Gem, finding that only one of them anticipated the surface field strength compatible with our observations. Results of our star spot mapping of YY Gem do not support the alternative family of theoretical stellar models which attempts to explain the radii inflation by postulating a large spot filling factor.

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“…This fact may arise from the different choices adopted for the calibration of stellar masses in the two catalogues. In our case, we adopted the calibration from Moya et al (2018) which accounts both for the temperature and absolute luminosity of the stars, while Stassun et al (2018) and Stassun et al (2019) adopt a calibration based only on the temperatures. The differences between the asPIC1.1 and TICv8 estimated parameters are shown in the histograms in Fig.…”

Section: Comparisonsmentioning

confidence: 99%

The all-sky PLATO input catalogue

Montalto

Piotto

Marrese

et al. 2021

A&A

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Context. The ESA PLAnetary Transits and Oscillations of stars (PLATO) mission will search for terrestrial planets in the habitable zone of solar-type stars. Because of telemetry limitations, PLATO targets need to be pre-selected. Aims. In this paper, we present an all sky catalogue that will be fundamental to selecting the best PLATO fields and the most promising target stars, deriving their basic parameters, analysing the instrumental performances, and then planing and optimising follow-up observations. This catalogue also represents a valuable resource for the general definition of stellar samples optimised for the search of transiting planets. Methods. We used Gaia Data Release 2 (DR2) astrometry and photometry and 3D maps of the local interstellar medium to isolate FGK (V≤13) and M (V≤16) dwarfs and subgiant stars. Results. We present the first public release of the all-sky PLATO Input Catalogue (asPIC1.1) containing a total of 2 675 539 stars including 2 378 177 FGK dwarfs and subgiants and 297 362 M dwarfs. The median distance in our sample is 428 pc for FGK stars and 146 pc for M dwarfs, respectively. We derived the reddening of our targets and developed an algorithm to estimate stellar fundamental parameters (T eff , radius, mass) from astrometric and photometric measurements. Conclusions. We show that the overall (internal+external) uncertainties on the stellar parameter determined in the present study are ∼230 K (4%) for the effective temperatures, ∼0.1 R (9%) for the stellar radii, and ∼0.1 M (11%) for the stellar mass. We release a special target list containing all known planet hosts cross-matched with our catalogue.

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Empirical Relations for the Accurate Estimation of Stellar Masses and Radii

Cited by 32 publications

References 55 publications

TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

Magnetic Field of the Eclipsing M-dwarf Binary YY Gem

The all-sky PLATO input catalogue

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