Theory of Spectroscopic and Eclipsing Binaries. Stellar Masses

1980 ◽  
pp. 241-281
Author(s):  
V. Kourganoff
Keyword(s):  
Eclipsing Binaries ◽  
Stellar Masses

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 Eclipsing binaries in the OGLE variable star catalogue: long-period evolved systems

2020 ◽  
Vol 496 (1) ◽  
pp. 550-563
Author(s):  
Barış Hoyman ◽  
Sara Bulut ◽  
Orkun Özdarcan ◽  
Ömür Çakırlı
Keyword(s):  
Stellar Evolution ◽  
Binary Stars ◽  
Eclipsing Binaries ◽  
Parameter Determination ◽  
Atmospheric Parameter ◽  
Physical Parameters ◽  
Giant Stars ◽  
Red Giant ◽  
Type Giant ◽  
Stellar Masses

ABSTRACT Red giant stars are proving to be an exceptional source of information for testing models of stellar evolution, as photometric and spectroscopic analysis has opened up a window into their interiors, providing an exciting chance to develop highly constrained stellar models. In this study, we present a determination of precise fundamental physical parameters belonging to five detached, double-lined, eclipsing binary stars in the Large and Small Magellanic Clouds containing G- or early K-type giant stars with extended envelopes. We also derived the distances to the systems by using a temperature–colour relation and compared these distances with the measurements provided in the literature. The measured stellar masses are in the range 1.8–3.0 M⊙ and comparison with the PAdova and TRieste Stellar Evolution Code (PARSEC) isochrones gives ages between 0.4 and 1.1 Gyr. The derived uncertainties for individual masses and radii of components are better than 3 and 7 per cent, respectively, for these systems. Additionally, we performed atmospheric parameter determination and [M/H] analysis for each, where we disentangled the spectra.

scholarly journals Modelling Kepler eclipsing binaries: homogeneous inference of orbital and stellar properties

2019 ◽  
Vol 489 (2) ◽  
pp. 1644-1666 ◽  
Author(s):  
D Windemuth ◽  
E Agol ◽  
A Ali ◽  
F Kiefer
Keyword(s):  
Main Sequence ◽  
Spectral Energy Distribution ◽  
Eclipsing Binaries ◽  
Spectral Energy ◽  
Parameter Estimates ◽  
Kepler Mission ◽  
Short Period ◽  
Show Evidence ◽  
Stellar Properties ◽  
Stellar Masses

Abstract We report on the properties of eclipsing binaries (EBs) from the Kepler mission with a newly developed photometric modelling code, which uses the light curve, spectral energy distribution of each binary, and stellar evolution models to infer stellar masses without the need for radial velocity (RV) measurements. We present solutions and posteriors to orbital and stellar parameters for 728 systems, forming the largest homogeneous catalogue of full Kepler binary parameter estimates to date. Using comparisons to published RV measurements, we demonstrate that the inferred properties (e.g. masses) are reliable for well-detached main-sequence (MS) binaries, which make up the majority of our sample. The fidelity of our inferred parameters degrades for a subset of systems not well described by input isochrones, such as short-period binaries that have undergone interactions, or binaries with post-MS components. Additionally, we identify 35 new systems which show evidence of eclipse timing variations, perhaps from apsidal motion due to binary tides or tertiary companions. We plan to subsequently use these models to search for and constrain the presence of circumbinary planets in Kepler EB systems.

scholarly journals Interferometric measurements of binaries

1997 ◽  
Vol 189 ◽  
pp. 109-114
Author(s):  
H.A. McAlister
Keyword(s):  
Binary Stars ◽  
Binary Star ◽  
Center Of Mass ◽  
Angular Separation ◽  
Eclipsing Binaries ◽  
Spectroscopic Binaries ◽  
Past Performance ◽  
Short Period ◽  
Stellar Masses

This paper is a brief overview of the past performance and future promise of interferometry as applied to the study of binary stars. For the sake of brevity, the important results from infrared techniques in recent years are regretfully omitted here. It is probably unnecessary to remind the reader that the analysis of binary star orbital motions is the only direct means for the determination of stellar masses. Historically, stellar masses have resulted primarily from orbits that are sufficiently wide in angular separation to permit the astrometric determination of the motions of the individual components about the center of mass as well as the parallax of the system or from short-period spectroscopic/eclipsing binaries. The advent of long baseline optical interferometers holds the promise of a wealth of new stellar mass data through the direct resolution of spectroscopic binaries.

scholarly journals Eclipsing Binaries as Precise Standard Candles and Distance Indicators

2005 ◽  
Vol 13 ◽  
pp. 454-454
Author(s):  
Jens Viggo Clausen
Keyword(s):  
Milky Way ◽  
Local Group ◽  
Eclipsing Binaries ◽  
Accurate Information ◽  
Direct Distance ◽  
Stellar Masses ◽  
Distance Indicators

Double-lined eclipsing binaries are (still) our main source for accurate information on stellar masses, radii, and luminosities. Also, they offer very direct distance determinations, useful within the Milky Way and for Local Group Galaxies. I will briefly review the methods involved and discuss critically their advantages and limitations. Furthermore, past and recent highlights will be presented.

scholarly journals Stellar Masses and Radii as Constraints on Stellar Models

1993 ◽  
Vol 137 ◽  
pp. 347-360
Author(s):  
Johannes Andersen
Keyword(s):  
Main Sequence ◽  
Eclipsing Binaries ◽  
Current Status ◽  
Sequence Evolution ◽  
Chemical Abundance ◽  
Tidal Interactions ◽  
Simple Question ◽  
Metal Abundance ◽  
Stellar Models ◽  
Stellar Masses

AbstractThe current status of empirical data on stellar masses and radii of sufficient accuracy to give constraints on stellar models is reviewed. Results from the best-studied eclipsing binaries can already trace the main-sequence evolution of 1-10 M⊙ stars in considerable detail and will be even more useful when supplemented by chemical abundance data.Taking the deceptively simple question of the observed width of the main sequence as an example, it is shown how careful attention to the details of the data is required to reach robust conclusions about such features of modern stellar evolution models as opacity tables or convective overshooting. Only detailed modelling of specific systems with known masses, radii, and metal abundance constrain the theory strongly enough that a truly critical test is achieved. The same is true when using tidal interactions in binaries (apsidal motion, rotational synchronization, and orbital circularization) as another probe into stellar interiors.

scholarly journals Detached Binaries in the Large Magellanic Cloud

2005 ◽  
Vol 13 ◽  
pp. 462-462
Author(s):  
G. Michalska ◽  
A. Pigulski
Keyword(s):  
Radial Velocity ◽  
Variable Star ◽  
Good Accuracy ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Light Curves ◽  
Distance Determination ◽  
Detached Binaries ◽  
Stellar Masses

Analysis of the radial-velocity and light curves of detached eclipsing binaries allows to derive stellar masses and radii and, in consequence, enables to find their distances. The method has been already applied to several LMC binaries, but in order to have the distance to the LMC determined with good accuracy, the parameters need to be known for a larger number of systems. As a first step we present results of the analysis of the photometry of over eighty detached binaries in the LMC selected from the OGLE-II catalog of 53 000 variable star candidates. If possible, we combine the OGLE-II data with the photometry from other projects (MACHO and EROS). As a result, we present the list of brightest eclipsing binaries in the LMC suitable for distance determination.

scholarly journals Sub-Milliarcsecond Binary Star Astrometry

1992 ◽  
Vol 135 ◽  
pp. 502-509 ◽  
Author(s):  
Xiaopei Pan ◽  
Michael Shao ◽  
M. Mark Colavita
Keyword(s):  
Binary Star ◽  
Primary Component ◽  
Eclipsing Binaries ◽  
Spectroscopic Binaries ◽  
Triple Systems ◽  
Long Baseline ◽  
Hyades Cluster ◽  
Stellar Masses ◽  
Binary Star System ◽  
Work Done

AbstractLong–baseline optical interferometry has revolutionised binary star astronomy. This paper reviews some recent binary star work done using the Mark III Stellar Interferometer. For the first time, many spectroscopic binaries, eclipsing binaries, triple systems, and binaries with X-ray sources have had their visual orbit, diameter of the primary component, and color index determined. Also, accurate stellar masses, distances, radii, and effective temperatures have been derived. A preliminary distance to the Hyades cluster has also been determined. In addition, preliminary observations provide evidence of a third body in the binary star system ζ Her, which may resolve an 85-year old discrepancy in astronomy.

scholarly journals The Araucaria project: High-precision orbital parallax and masses of eclipsing binaries from infrared interferometry

2019 ◽  
Vol 632 ◽  
pp. A31 ◽  
Author(s):  
A. Gallenne ◽  
G. Pietrzyński ◽  
D. Graczyk ◽  
B. Pilecki ◽  
J. Storm ◽  
...  
Keyword(s):  
Stellar Evolution ◽  
Binary Systems ◽  
Three Dimensional ◽  
Theoretical Models ◽  
Empirical Method ◽  
Eclipsing Binaries ◽  
Precision Level ◽  
Infrared Interferometry ◽  
The Masses ◽  
Stellar Masses

Context. The precise determinations of stellar mass at ≲1% provide important constraints on stellar evolution models. Accurate parallax measurements can also serve as independent benchmarks for the next Gaia data release. Aims. We measured the masses and distance of binary systems with a precision level better than 1% using a fully geometrical and empirical method. Methods. We obtained the first interferometric observations for the eclipsing systems AI Phe, AL Dor, KW Hya, NN Del, ψ Cen and V4090 Sgr with the VLTI/PIONIER combiner, which we combined with radial velocity measurements to derive their three-dimensional orbit, masses, and distance. Results. We determined very precise stellar masses for all systems, ranging in precision from 0.04% to 3.3%. We combined these measurements with the stellar effective temperature and linear radius to fit stellar isochrones models and determined the age of the systems. We also derived the distance to the systems with a precision level of 0.4%. Conclusions. The comparison of theoretical models with stellar parameters shows that stellar models are still deficient in simultaneously fitting the stellar parameters (Teff, R and M) with this level of precision on individual masses. This stresses the importance of precisely measuring the stellar parameters to better calibrate stellar evolution models. The precision of our model-independent orbital parallaxes varies from 24 μas as to 70 μas and the parallaxes provide a unique opportunity to verify whether the future Gaia measurements have systematic errors.

Magellanic Cloud Eclipsing Binaries: Primary Distance Indicators

1999 ◽  
Vol 190 ◽  
pp. 563-566
Author(s):  
J. D. Pritchard ◽  
W. Tobin ◽  
J. V. Clausen ◽  
E. F. Guinan ◽  
E. L. Fitzpatrick ◽  
...  
Keyword(s):  
New Zealand ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Fundamental Parameters ◽  
Distance Indicators

Our collaboration involves groups in Denmark, the U.S.A. Spain and of course New Zealand. Combining ground-based and satellite (IUEandHST) observations we aim to determine accurate and precise stellar fundamental parameters for the components of Magellanic Cloud Eclipsing Binaries as well as the distances to these systems and hence the parent galaxies themselves. This poster presents our latest progress.

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