HST/FGS Trigonometric Parallaxes of M-dwarf Eclipsing Binaries

What is known about the masses of main-sequence stars from the analysis of binary orbits? Double-lined eclipsing binaries are the main source of very precise stellar masses and radii (e.g. Andersen 1997), contributing more than 100 determinations with better than 2% precision over the range 0.6 to 20 Mʘ. For lower-mass stars we are forced to turn to nearby systems with astrometric orbits (e.g. Henry et al. 1993). Not only is the number of good mass determinations from such systems smaller, but also the precision is generally poorer. We are approaching an era when interferometers should have a major impact by supplying good astrometric orbits for dozens of double-lined systems. Already we are beginning to see the sorts of results to expect from this (e.g. Torres et al. 1997). Figure 1. Mass vs. absolute V magnitude for eclipsing binaries (circles) and nearby astrometric binaries (squares) Figure 1 is an updated version of a diagram presented by Henry et al. (1993, their Figure 2). It shows the general run of mass determinations from about 10 Mʘ down to the substellar limit near 0.075 Mʘ. Ninety of the points in Figure 1 are for eclipsing binary masses from Andersen’s review (1991) and are plotted as open circles. The results for eclipsing binaries published since 1991 are plotted as 30 filled circles, adopting the same limit of 2% for the mass precision. In most cases the uncertainties are similar to the size of the symbols. Especially noteworthy is the pair of new points for CM Draconis (Metcalfe et al. 1996) with masses near 0.25 Mʘ. Together with the points for YY Geminorum near 0.6 Mʘ, these are the only M dwarfs that have precise mass determinations. For the most part we are forced to rely on nearby stars with astrometric orbits, to fill in the M dwarf region of the diagram. We have used filled squares in Figure 1 for 29 such systems from Henry et al. (1993), updated using 14 new parallaxes from Hipparcos and 4 from the new Yale Parallax Catalog (1995). Gliese 508 is not included, because it is now known to be a triple, while Gliese 67AB, 570BC, and 623AB are not included because there are not yet any direct measurements of the V magnitude difference for these systems.

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Double-lined M dwarf eclipsing binaries from Catalina Sky Survey and LAMOST

Research in Astronomy and Astrophysics ◽

10.1088/1674-4527/17/2/15 ◽

2017 ◽

Vol 17 (2) ◽

pp. 15 ◽

Cited By ~ 3

Author(s):

Chien-Hsiu Lee ◽

Chien-Cheng Lin

Keyword(s):

Eclipsing Binaries ◽

Sky Survey ◽

M Dwarf

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Low-mass eclipsing binaries in the WFCAM Transit Survey: the persistence of the M-dwarf radius inflation problem

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/sty541 ◽

2018 ◽

Vol 476 (4) ◽

pp. 5253-5267 ◽

Cited By ~ 8

Author(s):

Patricia Cruz ◽

Marcos Diaz ◽

Jayne Birkby ◽

David Barrado ◽

Brigitta Sipöcz ◽

...

Keyword(s):

Eclipsing Binaries ◽

Low Mass ◽

M Dwarf

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Stability of planetary, single M dwarf, and binary star companions to Kepler detached eclipsing binaries and a possible five-body system

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2532 ◽

2020 ◽

Vol 498 (3) ◽

pp. 4356-4364

Author(s):

A K Getley ◽

B Carter ◽

R King ◽

S O’Toole

Keyword(s):

Binary Stars ◽

Binary Star ◽

Eclipsing Binaries ◽

Body System ◽

Star System ◽

Flip Flop ◽

Eclipsing Binary ◽

Photometric Monitoring ◽

Eclipsing Binary Star ◽

M Dwarf

ABSTRACT In this study, we identify 11 Kepler systems (KIC 5255552, 5653126, 5731312, 7670617, 7821010, 8023317, 10268809, 10296163, 11519226, 11558882, and 12356914) with a flip-flop effect in the eclipse timing variations O − C diagrams of the systems, report on what these systems have in common and whether these systems are dynamically stable. These systems have previously reported high eccentric binary stars with highly eccentric third bodies/outer companions. We find that all of the additional bodies in the system are dynamically stable for the configurations previously reported and are therefore likely to exist as described. We also provide additional evidence of KIC 5255552 being a quadruple star system composed of an eclipsing binary pair and non-eclipsing binary pair with the possibility of a fifth body in the system. With the advent of the NASA’s Transiting Exoplanet Survey Satellite (TESS) exoplanet survey, its precision photometric monitoring offers an opportunity to help confirm more local eclipsing binary star companions, including planets.

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CCD Parallaxes for Southern Very Low Luminosity Stars

Symposium - International Astronomical Union ◽

10.1017/s0074180900172961 ◽

1993 ◽

Vol 156 ◽

pp. 75-78

Author(s):

Philip A. Ianna

Keyword(s):

White Dwarfs ◽

Late Type ◽

M Dwarfs ◽

Dwarf Stars ◽

Ccd Observations ◽

Trigonometric Parallaxes ◽

M Dwarf Stars ◽

M Dwarf

Trigonometric parallaxes based on CCD observations are presented here for six southern very late-type M dwarf stars and three white dwarfs. The M dwarfs RG0050-2722, ESO207-61, MH2115-4518, MH2124-4228, and LHS3003 are among the very lowest luminosity stars known.

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M-dwarf Eclipsing Binaries with Flare Activity

The Astrophysical Journal ◽

10.3847/1538-4357/ab774a ◽

2020 ◽

Vol 892 (1) ◽

pp. 58

Author(s):

L.-C. Huang ◽

W.-H. Ip ◽

C.-L. Lin ◽

X.-L. Zhang ◽

Y.-H. Song ◽

...

Keyword(s):

Eclipsing Binaries ◽

Flare Activity ◽

M Dwarf

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Eclipsing Binaries: Precise Clocks to Detect Extrasolar Planets

Proceedings of the International Astronomical Union ◽

10.1017/s174392131301274x ◽

2012 ◽

Vol 8 (S293) ◽

pp. 165-167

Author(s):

Emil Kundra ◽

Theodor Pribulla ◽

Martin Vaňko ◽

Ľubomír Hambálek

Keyword(s):

White Dwarf ◽

Extrasolar Planets ◽

Ccd Camera ◽

Eclipsing Binaries ◽

List Type ◽

Object Selection ◽

Low Mass ◽

Selection For ◽

Orbital Periods ◽

M Dwarf

AbstractProject Dwarf is a new observing campaign focused on the detection of substellar companions to low-mass (composed of late-type, subdwarf (sd) or/and white dwarf (WD) components) detached eclipsing binaries using minima timing. The crucial condition for the object selection for this campaign is possibility to determine times of the minima with high precision. This is naturally fullfilled for eclipsing binaries with deep and narrow minima or systems hosting a WD component showing fast ingress or egress.The observing project includes three groups of close eclipsing binaries indicating presence of substellar circum-binary components: (i)systems with K or/and M dwarf components(ii)systems with hot subdwarf (sd) and M dwarf components(iii)systems with white dwarf (WD) component(s). The sample of the eclipsing systems have orbital periods in range of 0.1 to almost 3 days and their brightness fits possibilities of small telescopes equipped with a low-end CCD camera and at least VRI filter set. Such kind of telescopes allow us to develop observing network including also amateur astronomers.

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Empirical bolometric correction coefficients for nearby main-sequence stars in the Gaia era

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1659 ◽

2020 ◽

Vol 496 (3) ◽

pp. 3887-3905 ◽

Cited By ~ 2

Author(s):

Z Eker ◽

F Soydugan ◽

S Bilir ◽

V Bakış ◽

F Aliçavuş ◽

...

Keyword(s):

Main Sequence ◽

Eclipsing Binaries ◽

The Other ◽

Accurate Data ◽

Quadratic Relation ◽

Main Sequence Stars ◽

Data Release ◽

Trigonometric Parallaxes ◽

Bolometric Correction ◽

Intrinsic Colour

ABSTRACT Nearby detached double-lined eclipsing binaries with most accurate data were studied and 290 systems were found with at least one main-sequence component having a metallicity of 0.008 ≤ Z ≤ 0.040. Stellar parameters, light ratios, Gaia Data Release 2 trigonometric parallaxes, extinctions and/or reddening were investigated and only 206 systems were selected as eligible to calculate empirical bolometric corrections. NASA/IPAC Galactic dust maps were the main source of extinctions. Unreliable extinctions at low Galactic latitudes |b| ≤ 5° were replaced with individual determinations, if they exist in the literature, else associated systems were discarded. The main-sequence stars of te remaining systems were used to calculate the bolometric corrections (BCs) and to calibrate the BC–Teff relation, which is valid in the range 3100–36 000 K. De-reddened (B − V)0 colours, on the other hand, allowed us to calibrate two intrinsic colour–effective temperature relations; the linear one is valid for $T_{\rm eff}\gt 10\, 000$ K, while the quadratic relation is valid for $T_{\rm eff}\lt 10\, 000$ K; that is, both are valid in the same temperature range in which the BC–Teff relation is valid. New BCs computed from Teff and other astrophysical parameters are tabulated, as well.

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NGTS and WASP photometric recovery of a single-transit candidate from TESS

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz3212 ◽

2019 ◽

Cited By ~ 6

Author(s):

Samuel Gill ◽

Daniel Bayliss ◽

Benjamin F Cooke ◽

Peter J Wheatley ◽

Louise D Nielsen ◽

...

Keyword(s):

Radial Velocity ◽

Stellar Evolution ◽

Orbital Period ◽

Eclipsing Binaries ◽

Dwarf Star ◽

Velocity Measurements ◽

Eclipsing Binary ◽

Long Period ◽

M Dwarf

Abstract The Transiting Exoplanet Survey Satellite (TESS) produces a large number of single-transit event candidates, since the mission monitors most stars for only ∼27 days. Such candidates correspond to long-period planets or eclipsing binaries. Using the TESS Sector 1 full-frame images, we identified a 7750 ppm single-transit event with a duration of 7 hours around the moderately evolved F-dwarf star TIC-238855958 (Tmag=10.23, Teff=6280±85 K). Using archival WASP photometry we constrained the true orbital period to one of three possible values. We detected a subsequent transit-event with NGTS, which revealed the orbital period to be 38.20 d. Radial velocity measurements from the CORALIE Spectrograph show the secondary object has a mass of M2= 0.148 ± 0.003 M⊙, indicating this system is an F-M eclipsing binary. The radius of the M-dwarf companion is R2 = 0.171 ± 0.003 R⊙, making this one of the most well characterised stars in this mass regime. We find that its radius is 2.3-σ lower than expected from stellar evolution models.

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