scholarly journals Orbital Elements of MACHO Project Eclipsing Binary Stars

2005 ◽  
Vol 13 ◽  
pp. 467-467
Author(s):  
Charles Alcock
Keyword(s):  
Binary Stars ◽  
Large Scale ◽  
Major Axis ◽  
Orbital Elements ◽  
Semi Major Axis ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars ◽  
Large Numbers ◽  
Short Period ◽  
Velocity Information

Large scale photometric surveys can deliver very large numbers of eclipsing binary stars. It is not presently possible to obtain radial velocity information for more than a small fraction of these. We have made some progress in the estimation of the statistical distributions of orbital elements (including semi-major axis and eccentricity) in the MACHO Project catalog of eclipsing binary stars. We see the well-known tendency to circularization in short period orbits and also detect late tidal circularization during the giant phase. The extension of these techniques to newer surveys will also be discussed.

scholarly journals Turbulence in the Atmospheres of Eclipsing Binary Stars

1980 ◽  
Vol 51 ◽  
pp. 144-156
Author(s):  
K.O. Wright
Keyword(s):  
Binary Stars ◽  
Large Scale ◽  
Giant Component ◽  
Line Profiles ◽  
Eclipsing Binary ◽  
Multiple Structure ◽  
Eclipsing Binary Stars ◽  
Ultraviolet Observations ◽  
Chromospheric Structure ◽  
Lower Chromosphere

Abstract:A review of the orbits and dimensions of the ζ Aurigae systems is given, based on photometric and spectrographic observations. The Ca II K-line has been studied intensively to determine the extent and uneven structure of the chromospheres of these stars; the multiple structure of this line observed at several eclipses confirms the presence of large-scale clouds in the atmospheres. Measurements of line profiles and equivalent widths show that macroturbulent velocities up to 10 km/sec in the upper chromosphere, and up to 20 km/sec. in the lower chromosphere are present. Microturbulent velocities in the lower chromosphere are about 10 km/sec. Recent ultraviolet observations indicate that the B star in the 32 Cygni system may be within the outer chromosphere of the giant component and its radiation may affect the chromospheric structure more than had previously been suggested.

scholarly journals Photometric analysis of eclipsing binary stars

2019 ◽  
Vol 11 (20) ◽  
pp. 120-126
Author(s):  
Bushra Qassim AL-Abudi
Keyword(s):  
Computer Modeling ◽  
Binary Stars ◽  
Software Package ◽  
Eclipsing Binaries ◽  
Geometric Parameters ◽  
Photometric Analysis ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars ◽  
Short Period ◽  
Good Agreement

In this paper, photometric analysis of two short period group of the eclipsing binaries (RS CVn); RT And and BH Vir is presented. New physical and geometric parameters were obtained by performing two computer modeling. The first model is software package PHOEBE based on the Wilson–Devinney method, and the second is Binary Maker 3 (BM3).Our results are in good agreement with those obtained using the same modeling.

Searching for planets around eclipsing binary stars using timing method: NSVS 14256825

2017 ◽  
Vol 12 (S330) ◽  
pp. 405-406
Author(s):  
Ilham Nasiroglu ◽  
Krzysztof Goździewski ◽  
Aga Słowikowska ◽  
Krzysztof Krzeszowski ◽  
Michal Żejmo ◽  
...  
Keyword(s):  
Binary Stars ◽  
Brown Dwarf ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars ◽  
Short Period

AbstractWe present four new mid eclipse times and an updated O-C diagram of the short period eclipsing binary NSVS14256825. The new data follow the (O-C) trend and its model proposed in Nasiroglu et al. (2017). The (O-C) diagram shows quasi-periodic variations that can be explained with the presence of a brown-dwarf in a quasi-circular circumbinary orbit.

scholarly journals Statistics of Binary Stars: Semi-Major Axes

1976 ◽  
Vol 73 ◽  
pp. 369-379
Author(s):  
V. Trimble ◽  
C. Cheung
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Major Axis ◽  
Small Mass ◽  
Close Binaries ◽  
Mass Ratio ◽  
Orbital Elements ◽  
Semi Major Axis ◽  
Mass Ratios ◽  
Show Evidence

We have examined the distribution of the semi-major axes of the binary systems in the Sixth Catalogue of the Orbital Elements of Spectroscopic Binary Systems (and its extensions) and the correlation of semi-major axis with other properties of the systems. The total distribution has a single peak near asini=107km. Evolved systems have wider separations and smaller mass ratios than unevolved systems. Among each type separately, the distribution of mass ratios is bimodal and small mass ratio is correlated with large separation. These data appear to show evidence of two mechanisms of binary system formation and of the process of mass transfer in close binaries.

scholarly journals Light curve modeling of the short-period W UMa star GSC 02049-01164

2015 ◽  
Vol 11 (A29B) ◽  
pp. 536-539
Author(s):  
Lester Fox-Machado ◽  
Juan Echevarria ◽  
Diego González-Buitrago ◽  
Raul Michel
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Binary Stars ◽  
Binary Star ◽  
Major Axis ◽  
Physical Parameters ◽  
Semi Major Axis ◽  
San Pedro ◽  
Short Period ◽  
Curve Modeling

AbstractThe preliminary results of an analysis of the time-series photometric data of binary star GSC 02049-01164 (ROTSE1 J164341.65+251748.1) are presented. GSC 02049-01164 was observed for eight consecutive nights with the 0.84-m telescope of the San Pedro Martir Observatory in Mexico. The light curve of GSC 02049-01164 is typical of those of W UMa type binary stars. In an effort to gain a better understanding of the binary system and determine its physical properties we have analyzed the light curve with the software PHOEBE V.0 0.31a. We have found that GSC 02049-01164 binary system has a mass ratio of ~ 0.42, an inclination of ~ 85 degrees, a semi-major axis of ~ 2.24 R⊙. It is likely that the two stellar components are in contact, with a degree of overcontact of 13%. The physical parameters of the stellar components have been derived.

scholarly journals Testing convection in stellar models using detached eclipsing binaries

2006 ◽  
Vol 2 (S239) ◽  
pp. 157-159
Author(s):  
John Southworth ◽  
Hans Bruntt
Keyword(s):  
Binary Stars ◽  
Eclipsing Binaries ◽  
Eclipsing Binary ◽  
Fundamental Properties ◽  
Eclipsing Binary Stars ◽  
Average System ◽  
Stellar Models

AbstractThe fundamental properties of detached eclipsing binary stars can be measured very accurately, which could make them important objects for constraining the treatment of convection in theoretical stellar models. However, only four or five pieces of information can be found for the average system, which is not enough. We discuss studies of more interesting and useful objects: eclipsing binaries in clusters and eclipsing binaries with pulsating components.

scholarly journals A survey of eclipsing binary stars in the eastern spiral arm of M31

2005 ◽  
Vol 362 (3) ◽  
pp. 1006-1014 ◽  
Author(s):  
I. Todd ◽  
D. Pollacco ◽  
I. Skillen ◽  
D. M. Bramich ◽  
S. Bell ◽  
...  
Keyword(s):  
Binary Stars ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars ◽  
Spiral Arm

scholarly journals 22. The relation between orbits and physical characteristics of meteors

1968 ◽  
Vol 33 ◽  
pp. 217-235 ◽  
Author(s):  
Ľ. Kresák
Keyword(s):  
Major Axis ◽  
Progressive Increase ◽  
Physical Characteristics ◽  
The Other ◽  
Asteroid Belt ◽  
Angle Of Incidence ◽  
Semi Major Axis ◽  
Short Period ◽  
Broad Variety ◽  
Bona Fide

The relation of physical characteristics of meteors to their orbital elements is investigated using Harvard Super-Schmidt data. A set of characteristic indices is defined, allowing for the effects of geocentric velocity, angle of incidence, magnitude and mass, wherever a correction appears appropriate according to the correlations found by Jacchia et al. (1967). The medians for representative meteor samples are plotted in the semi-major axis/eccentricity diagram and the distribution of each parameter is derived. Although the differences are moderate compared to the measuring errors, six regions of different nature can be distinguished.The existence of two families of asteroidal meteors is indicated, one of them brought to crossing with the Earth's orbit by drag effects and the other by collision effects in the main asteroid belt. These meteors are characterized by low and uniform beginning heights, high fragmentation, low ablation, low deceleration, and bright wakes. A direct counterpart to this is represented by meteors moving in short-period orbits of higher eccentricity and shorter perihelion distance, which bear resemblance to the long-period and retrograde cometary meteors. Meteors with perihelion distances of less than 0·15 AU tend to resemble the bona fide asteroidal meteors by a progressive increase of fragmentation and decrease of reduced beginning heights and decelerations as the perihelion approaches the Sun. This is attributed to the selective destruction effects of solar radiation.With the exception of the Draconids, the mean characteristics of meteor showers agree well with those of sporadic meteors moving in similar orbits. It is suggested that the Draconid stream includes a broad variety of meteoric material and that the two peculiar Super-Schmidt meteors on record represent only the less resistive, short-lived component which has already been eliminated from the other showers.

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