Stellar Multiplicity Meets Stellar Evolution and Metallicity: The APOGEE View

Badenes, Carles; Mazzola, Christine N.; Thompson, Todd A.; Covey, Kevin R.; Freeman, Peter E.; Walker, Matthew G.; Moe, Maxwell; Troup, Nicholas; Nidever, David L.; Prieto, C. Allende; Andrews, Brett H.; Barbá, R. H.; Beers, Timothy C.; Bovy, Jo; Carlberg, Joleen K.; Lee, Nathan De; Johnson, Jennifer A.; Lewis, Hannah M.; Majewski, Steven R.; Pinsonneault, Marc H.; Sobeck, Jennifer; Stassun, Keivan G.; Stringfellow, Guy S.; Zasowski, Gail

doi:10.3847/1538-4357/aaa765

Cited by 160 publications

(181 citation statements)

References 87 publications

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“…This expected behaviour is indicative of longer periods for SB1s with a giant primary component. This trend is also reported in Badenes et al (2018), who thoroughly investigated the maximum RV range as a function of surface gravity and mass. They found a similar difference between dwarfs and giants.…”

Section: Orbital Propertiessupporting

confidence: 73%

“…comm.). 10 http://cdsxmatch.u-strasbg.fr/#tab=xmatch& 11 RAVE internal data release -292 stars in common with APOGEE (Badenes et al 2018). Since APOGEE (DR14) is a northern-hemisphere survey covering declinations above ∼ −32 • , the overlap is necessarily small (the GES maximum declination is ∼ 12 • ).…”

Section: Comparison With Other Surveysmentioning

confidence: 99%

“…Red and blue trends are almost superimposed. Yellow diamonds correspond to the SB1 fractions ofBadenes et al (2018) (see discussion in Sect. 4.4.7) centred on the median metallicities of their two samples covering a metallicity range illustrated by the yellow error bars.…”

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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: Orbital Propertiessupporting

confidence: 73%

Section: Comparison With Other Surveysmentioning

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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“…Recent studies have shown that the close-binary fraction (periods < 10 4 days; separation < 10 AU) increases with decreasing stellar metallicity (Grether & Lineweaver 2007;Yuan et al 2015;Badenes et al 2018;Moe et al 2019), consistent with formation of cose binaries due to disk fragmentation (Tanaka & Omukai 2014). While our eclipsing binary sample has periods much shorter than their close binaries, we investigate if our results can be explained by the metallicity dependence.…”

Section: Metallicitymentioning

confidence: 75%

Lifetime of short-period binaries measured from their Galactic kinematics

Hwang

Zakamska

2020

Monthly Notices of the Royal Astronomical Society

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As a significant fraction of stars are in multiple systems, binaries play a crucial role in stellar evolution. Among short-period (<1 day) binary characteristics, age remains one of the most difficult to measure. In this paper, we constrain the lifetime of short-period binaries through their kinematics. With the kinematic information from Gaia Data Release 2 and light curves from Wide-field Infrared Survey Explorer (WISE), we investigate the eclipsing binary fraction as a function of kinematics for a volumelimited main-sequence sample. We find that the eclipsing binary fraction peaks at a tangential velocity of 10 1.3−1.6 km s −1 , and decreases towards both low and high velocity end. This implies that thick disk and halo stars have eclipsing binary fraction 10 times smaller than the thin-disk stars. Using Galactic models, we show that our results are inconsistent with any known dependence of binary fraction on metallicity. Instead, our best-fit models suggest that the formation of these short-period binaries is delayed by 0.6-3 Gyr, and the disappearing time is less than the age of the thick disk. The delayed formation time of 0.6 Gyr is too long for any pre-main sequence interaction alone and is more consistent with the three-body interaction through the Kozai-Lidov mechanism and magnetic winds. Because the main-sequence lifetime of our sample is longer than 14 Gyr, if the disappearance of short-period binaries in the old population is due to their finite lifetime, our results imply that most ( 90%) short-period binaries in our sample are destroyed during their main-sequence stage.

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“…Recent surveys (Badenes et al 2018;Moe et al 2019) report an increase of the overall binary fraction of solar-type stars when metallicity decreases. The binary fraction at [Fe/H]=-1.0 is 40 ± 6% and reaches 53 ± 12% at [Fe/H]=-3.0 according to Moe et al (2019).…”

Section: Effect Of the Binary Mass Ratio Distributionmentioning

confidence: 99%

Impact of a companion and of chromospheric emission on the shape of chromosome maps for globular clusters

Martins

Morin

Charbonnel

et al. 2020

A&A

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Context. Globular clusters (GCs) host multiple populations of stars that are well-separated in a photometric diagram -the chromosome map -built from specific Hubble Space Telescope (HST) filters. Stars from different populations feature at various locations on this diagram due to peculiar chemical compositions. Stars of the first population, with field star-like abundances, sometimes show an unexpected extended distribution in the chromosome map. Aims. We aim to investigate the role of binaries and chromospheric emission on HST photometry of globular clusters' stars. We quantify their respective effects on the position of stars in the chromosome map, especially among the first population. Methods. We computed atmosphere models and synthetic spectra for stars of different chemical compositions, based on isochrones produced by stellar evolution calculations with abundance variations representative of first and second populations in globular clusters. From this we built synthetic chromosome maps for a mixture of stars of different chemical compositions. We subsequently replaced a fraction of stars with binaries, or stars with chromospheric emission, using synthetic spectroscopy. We studied how the position of stars is affected in the chromosome map. Results. Binaries can, in principle, explain the extension of the first population in the chromosome map. However, we find that given the binary fraction reported for globular clusters, the density of stars in the extended part is too small. Another difficulty of the binary explanation is that the shape of the distribution of the first population in the chromosome map is different in clusters with similar binary fractions. Also, the decrease of the binary fraction with radius is not mirrored in the shape of the chromosome map. Additionally, we find that the contribution of chromospheric emission lines to the HST photometry is too small to have an observable impact on the shape of the chromosome map. Continuum chromospheric emission has an effect qualitatively similar to binaries. Conclusions. We conclude that binaries do have an impact on the morphology of the chromosome map of globular clusters, but they are unlikely to explain entirely the shape of the extended distribution of the first population stars. Uncertainties in the properties of continuum chromospheric emission of stars in GCs prevent any quantitative conclusion. Therefore, the origin of the extended first population remains unexplained.

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Stellar Multiplicity Meets Stellar Evolution and Metallicity: The APOGEE View

Cited by 160 publications

References 87 publications

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

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

Lifetime of short-period binaries measured from their Galactic kinematics

Impact of a companion and of chromospheric emission on the shape of chromosome maps for globular clusters

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