scholarly journals Discovery and characterization of detached M dwarf eclipsing binaries in the WFCAM Transit Survey

2012 ◽  
Vol 426 (2) ◽  
pp. 1507-1532 ◽  
Author(s):  
Jayne Birkby ◽  
Bas Nefs ◽  
Simon Hodgkin ◽  
Gábor Kovács ◽  
Brigitta Sipőcz ◽  
...  
Keyword(s):  
Eclipsing Binaries ◽  
M Dwarf

scholarly journals The Mass-Luminosity Relation From Binaries

1998 ◽  
Vol 11 (1) ◽  
pp. 419-420
Author(s):  
David W. Latham
Keyword(s):  
Eclipsing Binaries ◽  
M Dwarfs ◽  
Direct Measurements ◽  
Nearby Stars ◽  
The Masses ◽  
Stellar Masses ◽  
M Dwarf ◽  
Magnitude Difference ◽  
Astrometric Binaries ◽  
Better Than

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.

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

2018 ◽  
Vol 476 (4) ◽  
pp. 5253-5267 ◽  
Author(s):  
Patricia Cruz ◽  
Marcos Diaz ◽  
Jayne Birkby ◽  
David Barrado ◽  
Brigitta Sipöcz ◽  
...  
Keyword(s):  
Eclipsing Binaries ◽  
Low Mass ◽  
M Dwarf

scholarly journals CHARACTERIZATION OF THE ATMOSPHERE OF THE HOT JUPITER HAT-P-32Ab AND THE M-DWARF COMPANION HAT-P-32B

2014 ◽  
Vol 796 (2) ◽  
pp. 115 ◽  
Author(s):  
Ming Zhao ◽  
Joseph G. O'Rourke ◽  
Jason T. Wright ◽  
Heather A. Knutson ◽  
Adam Burrows ◽  
...  
Keyword(s):  
M Dwarf ◽  
Hot Jupiter

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

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.

scholarly journals OMC/INTEGRAL photometric observations of pulsating components in eclipsing binaries and characterization of DY Aqr

2014 ◽  
Vol 443 (4) ◽  
pp. 3022-3032 ◽  
Author(s):  
J. Alfonso-Garzón ◽  
B. Montesinos ◽  
A. Moya ◽  
J. M. Mas-Hesse ◽  
S. Martín-Ruiz
Keyword(s):  
Eclipsing Binaries ◽  
Photometric Observations

scholarly journals The White Dwarf Binary Pathways Survey – IV. Three close white dwarf binaries with G-type secondary stars

2020 ◽  
Vol 501 (2) ◽  
pp. 1677-1689
Author(s):  
M S Hernandez ◽  
M R Schreiber ◽  
S G Parsons ◽  
B T Gänsicke ◽  
F Lagos ◽  
...  
Keyword(s):  
Spectral Type ◽  
White Dwarf ◽  
Binary Stars ◽  
Cataclysmic Variable ◽  
Common Envelope ◽  
History Of ◽  
Low Mass ◽  
Orbital Periods ◽  
M Dwarf

ABSTRACT Constraints from surveys of post-common envelope binaries (PCEBs) consisting of a white dwarf plus an M-dwarf companion have led to significant progress in our understanding of the formation of close white dwarf binary stars with low-mass companions. The white dwarf binary pathways project aims at extending these previous surveys to larger secondary masses, i.e. secondary stars of spectral-type AFGK. Here, we present the discovery and observational characterization of three PCEBs with G-type secondary stars and orbital periods between 1.2 and 2.5 d. Using our own tools as well as MESA, we estimate the evolutionary history of the binary stars and predict their future. We find a large range of possible evolutionary histories for all three systems and identify no indications for differences in common envelope evolution compared to PCEBs with lower mass secondary stars. Despite their similarities in orbital period and secondary spectral type, we estimate that the future of the three systems is very different: TYC 4962-1205-1 is a progenitor of a cataclysmic variable system with an evolved donor star, TYC 4700-815-1 will run into dynamically unstable mass transfer that will cause the two stars to merge, and TYC 1380-957-1 may appear as supersoft source before becoming a rather typical cataclysmic variable star.

scholarly journals HST/FGS Trigonometric Parallaxes of M-dwarf Eclipsing Binaries

2020 ◽  
Vol 132 (1011) ◽  
pp. 054201
Author(s):  
Gerard T. van Belle ◽  
Gail H. Schaefer ◽  
Kaspar von Braun ◽  
Edmund P. Nelan ◽  
Zachary Hartman ◽  
...  
Keyword(s):  
Eclipsing Binaries ◽  
Trigonometric Parallaxes ◽  
M Dwarf

Characterization of eclipsing binaries in High Latitude Field 356

New Astronomy ◽  
2019 ◽  
Vol 67 ◽  
pp. 53-66
Author(s):  
Derck P. Smits ◽  
P.L. Skelton
Keyword(s):  
High Latitude ◽  
Eclipsing Binaries

scholarly journals The CARMENES search for exoplanets around M dwarfs

2019 ◽  
Vol 627 ◽  
pp. A161 ◽  
Author(s):  
V. M. Passegger ◽  
A. Schweitzer ◽  
D. Shulyak ◽  
E. Nagel ◽  
P. H. Hauschildt ◽  
...  
Keyword(s):  
Stellar Atmosphere ◽  
Stellar Atmospheres ◽  
M Dwarfs ◽  
Fundamental Parameters ◽  
Visible Spectra ◽  
New Equation ◽  
First Time ◽  
M Dwarf ◽  
Recent Version

We present precise photospheric parameters of 282 M dwarfs determined from fitting the most recent version of PHOENIX models to high-resolution CARMENES spectra in the visible (0.52–0.96μm) and NIR wavelength range (0.96–1.71μm). With its aim to search for habitable planets around M dwarfs, several planets of different masses have been detected. The characterization of the target sample is important for the ability to derive and constrain the physical properties of any planetary systems that are detected. As a continuation of previous work in this context, we derived the fundamental stellar parameters effective temperature, surface gravity, and metallicity of the CARMENES M-dwarf targets from PHOENIX model fits using aχ2method. We calculated updated PHOENIX stellar atmosphere models that include a new equation of state to especially account for spectral features of low-temperature stellar atmospheres as well as new atomic and molecular line lists. We show the importance of selecting magnetically insensitive lines for fitting to avoid effects of stellar activity in the line profiles. For the first time, we directly compare stellar parameters derived from multiwavelength range spectra, simultaneously observed for the same star. In comparison with literature values we show that fundamental parameters derived from visible spectra and visible and NIR spectra combined are in better agreement than those derived from the same spectra in the NIR alone.

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