Eclipsing Stars

1985 ◽  
pp. 198-220 ◽  
Author(s):  
Cuno Hoffmeister ◽  
Gerold Richter ◽  
Wolfgang Wenzel
Keyword(s):  
Eclipsing Stars

Minima and periods of eclipsing stars.

1959 ◽  
Vol 64 ◽  
pp. 258 ◽  
Author(s):  
B. S. Whitney
Keyword(s):  
Eclipsing Stars

Ephemerides of eclipsing stars.

1963 ◽  
Vol 68 ◽  
pp. 257 ◽  
Author(s):  
B. D. Wood ◽  
J. E. Forbes
Keyword(s):  
Eclipsing Stars

scholarly journals Eclipsing Binaries in the LMC: a Wealth of Data for Astrophysical Tests

2006 ◽  
Vol 2 (S240) ◽  
pp. 377-379
Author(s):  
A. Derekas ◽  
L. L. Kiss ◽  
T. R. Bedding
Keyword(s):  
Large Magellanic Cloud ◽  
Variable Stars ◽  
Period Change ◽  
Eclipsing Binaries ◽  
Third Body ◽  
Orbital Inclination ◽  
Eclipsing Stars ◽  
Period Distribution ◽  
New Period ◽  
Clean Sample

AbstractWe have analysed publicly available MACHO observations of 6833 variable stars in the Large Magellanic Cloud, classified as eclipsing binaries. After finding that a significant fraction of the sample was misclassified, we redetermined periods and variability class for all stars, producing a clean sample of 3031 eclipsing binaries. We have investigated their distribution in the period-color-luminosity space, which was used, for example, to assign a foreground probability to every object and establish new period-luminosity relations to selected types of eclipsing stars. We found that the orbital period distribution of LMC binaries is very similar to those of the SMC and the Milky Way. We have also determined the rate of period change for every star using the O-C method, discovering about 40 eclipsing binaries with apsidal motion, 45 systems with cyclic period changes and about 80 stars with parabolic O-C diagrams. In a few objects we discovered gradual amplitude variation, which can be explained by changes in the orbital inclination caused by a perturbing third body in the system.

scholarly journals Eclipsing Binaries in the Magellanic Clouds

2005 ◽  
Vol 13 ◽  
pp. 451-451
Author(s):  
Andrzej Udalski
Keyword(s):  
Gravitational Lensing ◽  
Direct Determination ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Physical Parameters ◽  
Second Phase ◽  
Internet Archive ◽  
Pulsating Stars ◽  
Eclipsing Stars

We present results of a search for eclipsing binaries in the Magellanic Cloud fields covering central parts of these galaxies. The data were collected during the second phase of the Optical Gravitational Lensing Experiment survey (OGLE-II) in 1997-2000. In total, about 1500 and 3000 eclipsing stars were found in the Small and Large Magellanic Cloud, respectively (Udalski et al. 1998, Wyrzykowski et al. 2003). The photometric data of all objects are available to the astronomical community from the OGLE Internet archive (http://sirius.astrouw.edu.pl/~ogle/). OGLE-II data contain a full variety of classical eclipsing objects of all types: Algol EA-type, β-Lyr EB-type and W UMA EW-type stars. Large samples of stars allow to study in detail statistical properties of eclipsing objects. OGLE data also contain many very unusual eclipsing stars. Examples include eclipsing variable B-type stars (Mennickent et al. 2003), many spotted stars or eclipsing stars with a Cepheid as a component (Udalski et al. 1999). Recently three objects from the LMC revealing simultaneously RR Lyr and eclipsing binary type variability were discovered (Soszyński et al 2003). If the follow-up observations confirm that both components are physically bound and not optical blends these stars will provide a unique opportunity of direct determination of physical parameters of RR Lyr pulsating stars.

scholarly journals New light elements for selected eclipsing stars.

1951 ◽  
Vol 56 ◽  
pp. 53 ◽  
Author(s):  
Frank Bradshaw Wood
Keyword(s):  
Light Elements ◽  
Eclipsing Stars

Narrow-band photometric classification of eclipsing binaries

1966 ◽  
Vol 24 ◽  
pp. 190-210
Author(s):  
D. H. McNamara
Keyword(s):  
Temperature Scale ◽  
Narrow Band ◽  
Eclipsing Binaries ◽  
Spectral Classification ◽  
Uniform System ◽  
Fundamental Properties ◽  
Eclipsing Stars ◽  
Accurate Knowledge ◽  
Observational Program

Although a great deal of work has been devoted in recent years to the problem of improving our knowledge of the spectroscopic and light elements of the eclipsing stars, little effort has been expended on the problem of two-dimensional spectral classification of the component stars on a uniform system. The only serious attempt in this direction appears to be the MK classification of a number of eclipsing stars by Miss Roman (i). Since the light- and velocity-curves of eclipsing systems provide us with fundamental properties such as radii, masses, and densities it is extremely important to have accurate knowledge of the luminosities and spectral types of these objects. In this paper we describe the results of an observational program designed specifically to improve our knowledge of the luminosities and colors of these important stars. The luminosities and colors are then utilized in a discussion of the mass-luminosity relation and effective-temperature scale of stars brigher than the Sun.

Minima of eclipsing stars.

1964 ◽  
Vol 69 ◽  
pp. 316 ◽  
Author(s):  
W. S. Fitch
Keyword(s):  
Eclipsing Stars

scholarly journals Fundamental properties of the pre-main sequence eclipsing stars of MML 53 and the mass of the tertiary

2019 ◽  
Vol 623 ◽  
pp. A23 ◽  
Author(s):  
Y. Gómez Maqueo Chew ◽  
L. Hebb ◽  
H. C. Stempels ◽  
A. Paat ◽  
K. G. Stassun ◽  
...  
Keyword(s):  
Close Binary ◽  
Formation Mechanisms ◽  
Primary Star ◽  
Eclipsing Binary ◽  
Secondary Star ◽  
The Third ◽  
Eclipsing Stars ◽  
Systemic Velocity ◽  
Outer Component ◽  
The Masses

We present the most comprehensive analysis to date of the Upper Centaurus Lupus eclipsing binary MML 53 (with PEB = 2.097892 d), and for the first time, confirm the bound-nature of the third star (in a P3 ∼ 9 yr orbit) by constraining its mass dynamically. Our analysis is based on new and archival spectra and time-series photometry, spanning 80% of one orbit of the outer component. From the spectroscopic analysis, we determined the temperature of the primary star to be 4880 ± 100 K. The study of the close binary incorporated treatment of spots and dilution by the tertiary in the light curves, allowing for the robust measurement of the masses of the eclipsing components within 1% (M1 = 1.0400 ± 0.0067 M⊙ and M2 = 0.8907 ± 0.0058 M⊙), their radii within 4.5% (R1 = 1.283 ± 0.043 R⊙ and R2 = 1.107 ± 0.049 R⊙), and the temperature of the secondary star (Teff, 2 = 4379 ± 100 K). From the analysis of the eclipse timings, and the change in systemic velocity of the eclipsing binary and the radial velocities of the third star, we measured the mass of the outer companion to be 0.7 M⊙ (with a 20% uncertainty). The age we derived from the evolution of the temperature ratio between the eclipsing components is fully consistent with previous, independent estimates of the age of Upper Centaurus Lupus (16 ± 2 Myr). At this age, the tightening of the MML 53 eclipsing binary has already occurred, thus supporting close-binary formation mechanisms that act early in the stars’ evolution. The eclipsing components of MML 53 roughly follow the same theoretical isochrone, but appear to be inflated in radius (by 20% for the primary and 10% for the secondary) with respect to recent evolutionary models. However, our radius measurement of the 1.04 M⊙ primary star of MML 53 is in full agreement with the independent measurement of the secondary of NP Per which has the same mass and a similar age. The eclipsing stars of MML 53 are found to be larger but not cooler than predicted by non-magnetic models, it is not clear what is the mechanism that is causing the radius inflation given that activity, spots and/or magnetic fields slowing their contraction, require the inflated stars to be cooler to remain in thermal equilibrium.

scholarly journals Fundamental properties of the pre-main sequence eclipsing stars of MML 53 and the mass of the tertiary

2019 ◽  
Vol 623 ◽  
pp. A23
Author(s):  
Y. Gómez Maqueo Chew ◽  
L. Hebb ◽  
H. C. Stempels ◽  
A. Paat ◽  
K. G. Stassun ◽  
...  
Keyword(s):  
Close Binary ◽  
Formation Mechanisms ◽  
Primary Star ◽  
Eclipsing Binary ◽  
Secondary Star ◽  
The Third ◽  
Eclipsing Stars ◽  
Systemic Velocity ◽  
Outer Component ◽  
The Masses

We present the most comprehensive analysis to date of the Upper Centaurus Lupus eclipsing binary MML 53 (with PEB = 2.097892 d), and for the first time, confirm the bound-nature of the third star (in a P3 ∼ 9 yr orbit) by constraining its mass dynamically. Our analysis is based on new and archival spectra and time-series photometry, spanning 80% of one orbit of the outer component. From the spectroscopic analysis, we determined the temperature of the primary star to be 4880 ± 100 K. The study of the close binary incorporated treatment of spots and dilution by the tertiary in the light curves, allowing for the robust measurement of the masses of the eclipsing components within 1% (M1 = 1.0400 ± 0.0067 M⊙ and M2 = 0.8907 ± 0.0058 M⊙), their radii within 4.5% (R1 = 1.283 ± 0.043 R⊙ and R2 = 1.107 ± 0.049 R⊙), and the temperature of the secondary star (Teff, 2 = 4379 ± 100 K). From the analysis of the eclipse timings, and the change in systemic velocity of the eclipsing binary and the radial velocities of the third star, we measured the mass of the outer companion to be 0.7 M⊙ (with a 20% uncertainty). The age we derived from the evolution of the temperature ratio between the eclipsing components is fully consistent with previous, independent estimates of the age of Upper Centaurus Lupus (16 ± 2 Myr). At this age, the tightening of the MML 53 eclipsing binary has already occurred, thus supporting close-binary formation mechanisms that act early in the stars’ evolution. The eclipsing components of MML 53 roughly follow the same theoretical isochrone, but appear to be inflated in radius (by 20% for the primary and 10% for the secondary) with respect to recent evolutionary models. However, our radius measurement of the 1.04 M⊙ primary star of MML 53 is in full agreement with the independent measurement of the secondary of NP Per which has the same mass and a similar age. The eclipsing stars of MML 53 are found to be larger but not cooler than predicted by non-magnetic models, it is not clear what is the mechanism that is causing the radius inflation given that activity, spots and/or magnetic fields slowing their contraction, require the inflated stars to be cooler to remain in thermal equilibrium.

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