scholarly journals Eclipsing Binary Stars from Space

2006 ◽  
Vol 2 (S240) ◽  
pp. 624-627
Author(s):  
Hans Bruntt ◽  
John Southworth
Keyword(s):  
Light Curve ◽  
High Precision ◽  
Binary Stars ◽  
Primary Component ◽  
Wide Field ◽  
Small Aperture ◽  
Eclipsing Binary ◽  
Preliminary Results ◽  
Eclipsing Binary Stars

AbstractWe have begun a programme to obtain high-precision photometry of bright detached eclipsing binary (dEB) stars with the Wide-field InfraRed Explorer (WIRE) satellite (Bruntt & Buzasi 2006). Due to the small aperture of WIRE, only stars brighter than V = 6 can be observed. We are collecting data for about a dozen dEB targets and here we present preliminary results for three of them. We have chosen dEBs with primary components of B and early A type. One of our aims is to combine the information from the light curve analyses of the eclipses with asteroseismic information from analysis of the pulsation of the primary component.

scholarly journals A New Binary Star System of EW Type in Draco: GSC 03905-01870

2018 ◽  
Author(s):  
Salvador Barquin
Keyword(s):  
Light Curve ◽  
Binary Stars ◽  
Variable Star ◽  
Binary Star ◽  
Type I ◽  
Star System ◽  
Primary Minimum ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars ◽  
Binary Star System

Discovery of a new binary star system (GSC 03905-01870 = USNO-B1.0 1431-0327922 = UCAC4 716-059522) in the Draco constellation is presented. It was discovered during a search for previously unreported eclipsing binary stars through the ASAS-SN database. The shape of the light curve and its characteristics (period of 0.428988±0.000001 d, amplitude of 0.34±0.02 V Mag, primary minimum epoch HJD 2457994.2756±0.0002) indicates that the new variable star is an eclipsing binary of W Ursae Majoris type. I registered this variable star in The International Variable Star Index (VSX), its AAVSO UID is 000-BMP-891.

scholarly journals The TESS light curve of AI Phoenicis

2020 ◽  
Vol 498 (1) ◽  
pp. 332-343 ◽  
Author(s):  
P F L Maxted ◽  
Patrick Gaulme ◽  
D Graczyk ◽  
K G Hełminiak ◽  
C Johnston ◽  
...  
Keyword(s):  
Light Curve ◽  
Binary Stars ◽  
Model Parameters ◽  
Multiple Sources ◽  
Light Curve Analysis ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars ◽  
Free Parameters ◽  
The Masses ◽  
Stellar Masses

ABSTRACT Accurate masses and radii for normal stars derived from observations of detached eclipsing binary stars are of fundamental importance for testing stellar models and may be useful for calibrating free parameters in these model if the masses and radii are sufficiently precise and accurate. We aim to measure precise masses and radii for the stars in the bright eclipsing binary AI Phe, and to quantify the level of systematic error in these estimates. We use several different methods to model the Transiting Exoplanet Survey Satellite (TESS) light curve of AI Phe combined with spectroscopic orbits from multiple sources to estimate precisely the stellar masses and radii together with robust error estimates. We find that the agreement between different methods for the light-curve analysis is very good but some methods underestimate the errors on the model parameters. The semi-amplitudes of the spectroscopic orbits derived from spectra obtained with modern échelle spectrographs are consistent to within 0.1 per cent. The masses of the stars in AI Phe are $M_1 = 1.1938 \pm 0.0008\, \rm M_{\odot }$ and $M_2 = 1.2438 \pm 0.0008\, \rm M_{\odot }$, and the radii are $R_1 = 1.8050 \pm 0.0022\, \rm R_{\odot }$ and $R_2 = 2.9332 \pm 0.0023\, \rm R_{\odot }$. We conclude that it is possible to measure accurate masses and radii for stars in bright eclipsing binary stars to a precision of 0.2 per cent or better using photometry from TESS and spectroscopy obtained with modern échelle spectrographs. We provide recommendations for publishing masses and radii of eclipsing binary stars at this level of precision.

Searching for pulsations in Kepler eclipsing binary stars

2013 ◽  
Vol 9 (S301) ◽  
pp. 413-414 ◽  
Author(s):  
Patrick Gaulme ◽  
Joyce A. Guzik
Keyword(s):  
Fourier Analysis ◽  
Light Curve ◽  
Binary Stars ◽  
Binary Systems ◽  
High Amplitude ◽  
Eclipsing Binaries ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars ◽  
Scuti Star ◽  
Additional Constraints

AbstractEclipsing binaries can in principle provide additional constraints to facilitate asteroseismology of one or more pulsating components. We have identified 94 possible eclipsing binary systems in a sample of over 1800 stars observed in long cadence as part of the Kepler Guest Observer Program to search for γ Doradus and δ Scuti star candidates. We show the results of a procedure to fold the light curve to identify the potential binary period, subtract a fit to the binary light curve, and perform a Fourier analysis on the residuals to search for pulsation frequencies that may arise in one or both of the stellar components. From this sample, we have found a large variety of light curve types; about a dozen stars show frequencies consistent with δ Sct or γ Dor pulsations, or light curve features possibly produced by stellar activity (rotating spots). For several stars, the folded candidate ‘binary’ light curve resembles more closely that of an RR Lyr, Cepheid, or high-amplitude δ Sct star. We show highlights of our results and discuss the potential for asteroseismology of the most interesting objects.

scholarly journals High Resolution Interferometric Observations of Eclipsing Binary Stars

1994 ◽  
Vol 158 ◽  
pp. 413-415
Author(s):  
Xiaopei Pan ◽  
Michael Shao ◽  
M. Mark Colavita
Keyword(s):  
Binary Stars ◽  
Primary Component ◽  
High Angular Resolution ◽  
Reliable Determination ◽  
Eclipsing Binary ◽  
Orbital Parameters ◽  
Eclipsing Stars ◽  
Stellar Interferometer ◽  
Eclipsing Binary Stars ◽  
Systematic Uncertainties

Eclipsing binary stars are of great importance in astronomy. Now, high angular resolution measurements of eclipsing stars with the Mark III Stellar Interferometer (Shao 1988) can determine not only all of the orbital parameters, but also the luminosities and color indices of the two components, and can yield precise information for the study of the stellar evolution models. Particularly, the combination of interferometric and photometric results provide a direct measurement of stellar effective temperature. In the case where the primary component can be resolved, the results from the optical interferometer then provide a reliable determination of the absolute system parameters. In addition, eclipsing binary stars are good candidates for comparison of different techniques, i.e., interferometric, photometric, astrometric, and spectroscopic, and for checking whether systematic uncertainties exist with certain techniques.

scholarly journals Eclipsing binary stars with extreme light curve asymmetries mined from large astronomical surveys

2017 ◽  
Vol 152 ◽  
pp. 03010
Author(s):  
Athanasios Papageorgiou ◽  
Georgios Kleftogiannis ◽  
Panagiota-Eleftheria Christopoulou
Keyword(s):  
Light Curve ◽  
Binary Stars ◽  
Eclipsing Binary ◽  
Astronomical Surveys ◽  
Eclipsing Binary Stars

scholarly journals Photometry of Eclipsing Binary Stars in the Large and Small Magellanic Clouds

2004 ◽  
Vol 191 ◽  
pp. 116-120
Author(s):  
G.P. Bayne ◽  
W. Tobin ◽  
J.D. Pritchard ◽  
I. Bond ◽  
K.R. Pollard ◽  
...  
Keyword(s):  
Binary Stars ◽  
Primary Component ◽  
Magellanic Clouds ◽  
Eclipsing Binaries ◽  
Light Curves ◽  
Circular Orbits ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars

AbstractThe light curves for three eclipsing binaries in the Magellanic Clouds have been obtained using CCD uVJIC photometry. One target in the LMC, MACHO*05:36:48.7−69:17:00, is an eccentric system, e = 0.20, with a period of 3.853534 ± 0.000005 d. Initial solutions indicate a primary component in the range Teff,1 = 20,000−35,000K and the secondary Teff,2 1000−2000K cooler than the primary, with inclinations ranging i = 84.2° − 86.0°. Two targets in the SMC, MOA J005018.4-723855 and MOA J005623.5−722123, have periods of 1.8399±0.0004 and 2.3199 ± 0.0003 days respectively. Both have circular orbits with the former being a semi-detached system.

Photometric study of two eclipsing binary stars: Light curve analysis and system parameters for GU CMa and SWASP J011732.10+525204.9

New Astronomy ◽  
2018 ◽  
Vol 59 ◽  
pp. 8-13 ◽  
Author(s):  
A. Shokry ◽  
S.M. Saad ◽  
M.A. Hamdy ◽  
M.M. Beheary ◽  
M.S. Abolazm ◽  
...  
Keyword(s):  
Light Curve ◽  
Binary Stars ◽  
Curve Analysis ◽  
Photometric Study ◽  
Light Curve Analysis ◽  
Eclipsing Binary ◽  
System Parameters ◽  
Eclipsing Binary Stars

The Eclipsing Binary WX Eridani

1979 ◽  
Vol 46 ◽  
pp. 385
Author(s):  
M.B.K. Sarma ◽  
K.D. Abhankar
Keyword(s):  
Light Curve ◽  
Spectral Type ◽  
Orbital Period ◽  
Primary Component ◽  
Light Curves ◽  
Absorption Feature ◽  
Primary Star ◽  
Eclipsing Binary ◽  
The Times ◽  
Phase Angles

AbstractThe Algol-type eclipsing binary WX Eridani was observed on 21 nights on the 48-inch telescope of the Japal-Rangapur Observatory during 1973-75 in B and V colours. An improved period of P = 0.82327038 days was obtained from the analysis of the times of five primary minima. An absorption feature between phase angles 50-80, 100-130, 230-260 and 280-310 was present in the light curves. The analysis of the light curves indicated the eclipses to be grazing with primary to be transit and secondary, an occultation. Elements derived from the solution of the light curve using Russel-Merrill method are given. From comparison of the fractional radii with Roche lobes, it is concluded that none of the components have filled their respective lobes but the primary star seems to be evolving. The spectral type of the primary component was estimated to be F3 and is found to be pulsating with two periods equal to one-fifth and one-sixth of the orbital period.

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