scholarly journals WASP light curve of the eclipsing binary VZ CVn

2012 ◽  
pp. 77-82 ◽  
Author(s):  
O. Latkovic
Keyword(s):  
Light Curve ◽  
Radial Velocity ◽  
Eclipsing Binary ◽  
Spectroscopic Parameters ◽  
Orbital Parameters ◽  
Minimum Light ◽  
Photometric Elements ◽  
Modeling Code

The WASP light curve of the eclipsing binary VZ CVn, consisting of more than 14000 individual observations, is analyzed for photometric elements using the modeling code of Djurasevic (1992). The spectroscopic parameters are adopted from the recent radial velocity work by Pribulla et al. (2009). The results of the study include new times of minimum light, an improved ephemeris, and the updated physical and orbital parameters of the system.

scholarly journals Spectroscopic Orbit of the Eclipsing Binary BD +52°2009

1999 ◽  
Vol 170 ◽  
pp. 325-330
Author(s):  
B. Khalesseh
Keyword(s):  
Correlation Function ◽  
Light Curve ◽  
Radial Velocity ◽  
Physical Model ◽  
Cross Correlation ◽  
Cross Correlation Function ◽  
Physical Parameters ◽  
Mass Ratio ◽  
Velocity Measurements ◽  
Eclipsing Binary

AbstractNew radial velocity measurements of the Algol-type eclipsing binary BD +52 °2009, based on Reticon observations, are presented. The velocity measures are based on fitting theoretical profiles, generated by a physical model of the binary, to the observed cross-correlation function (ccf). Such profiles match this function very well, much better in fact than Gaussian profiles, which are generally used. Measuring the ccf’s with Gaussian profiles yields the following results: mp sin3i = 2.55 ± 0.05m⊙, ms sin3i = 1.14 ± 0.03m⊙, (ap + as) sin i = 7.34 ± 0.05R⊙, and mp/ms = 2.23 ± 0.05. However, measuring the ccf’s with theoretical profiles yields a mass ratio of 2.33 and following results: mp sin3i = 2.84 ± 0.05m⊙, ms sin3i = 1.22 ± 0.03m⊙, (ap + as) sin i = 7.56 ± 0.05R⊙. The system has a semi-detached configuration. By combining the solution of a previously published light curve with the spectroscopic orbit, one can obtain the following physical parameters: mp = 2.99m⊙, ms3 = 1.28m⊙, < Tp >= 9600K, < Ts >= 5400K, < Rp >= 2.35R⊙, < Rs >= 2.12R⊙. The system consists of an A0 primary and a G2 secondary.

scholarly journals Fluorescence and Chromospheric Activity of V471 Tau

2002 ◽  
Vol 187 ◽  
pp. 167-172
Author(s):  
T.R. Vaccaro ◽  
R.E. Wilson
Keyword(s):  
Light Curve ◽  
Radial Velocity ◽  
Orbital Period ◽  
White Dwarf ◽  
Binary Star ◽  
Star Model ◽  
Orbital Inclination ◽  
Orbital Parameters ◽  
Maximum Emission ◽  
Chromospheric Activity

AbstractThe red dwarf + white dwarf eclipsing binary V471 Tau shows a variable Hα feature that varies from absorption during eclipse to maximum emission during white dwarf transit. In 1998 we obtained simultaneous BVRI photometry and Hα spectroscopy, with thorough phase coverage of the 12.5 hour orbital period. A binary star model was used with our light curve, radial velocity, and Hα data to refine stellar and orbital parameters. Combined absorption-emission profiles were generated by the model and fit to the observations, yielding a red star radius of 0.94R⊙. Orbital inclination 78° is required with this size and other known parameters. The model includes three spots 1,000 K cooler than the surrounding photosphere. The variable Hα profile was modeled as a chromospheric fluorescing region (essentially on the surface of the red star) centered at the substellar point. Additional emission seen outside our modeled profiles may be large co-rotating prominences that complicate the picture.

scholarly journals Light Curve and Orbital Period Analysis of the Eclipsing Binary AT Peg

2011 ◽  
Vol 7 (S282) ◽  
pp. 55-56
Author(s):  
Alexios Liakos ◽  
Panagiotis Niarchos ◽  
Edwin Budding
Keyword(s):  
Light Curve ◽  
Orbital Period ◽  
Time Effect ◽  
Light Curves ◽  
Period Analysis ◽  
Eclipsing Binary ◽  
Secular Changes ◽  
Photometric Observations ◽  
Photometric Elements

AbstractCCD photometric observations of the Algol-type eclipsing binary AT Peg have been obtained. The light curves are analyzed with modern techniques and new geometric and photometric elements are derived. A new orbital period analysis of the system, based on the most reliable timings of minima found in the literature, is presented and apparent period modulations are discussed with respect to the Light-Time effect (LITE) and secular changes in the system. The results of these analyses are compared and interpreted in order to obtain a coherent view of the system's behaviour.

scholarly journals A search for pulsations in two Algol-type systems V1241 Tau and GQ Dra

2013 ◽  
Vol 9 (S301) ◽  
pp. 507-508 ◽  
Author(s):  
Burak Ulaş ◽  
Ceren Ulusoy ◽  
Kosmas Gazeas ◽  
Naci Erkan ◽  
Alexios Liakos
Keyword(s):  
Light Curve ◽  
Binary Systems ◽  
Type Systems ◽  
Light Variation ◽  
Light Curves ◽  
Eclipsing Binary ◽  
Photometric Observations ◽  
Fourier Techniques ◽  
Photometric Elements

AbstractWe present new photometric observations of two eclipsing binary systems, V1241 Tau and GQ Dra. We use the following methodology: initially, the Wilson-Devinney code is applied to the light curves in order to determine the photometric elements of the systems. Then, the residuals are analysed using Fourier techniques. The results are the following. One frequency can be possibly attributed to a real light variation of V1241 Tau, while there is no evidence of pulsations in the light curve of GQ Dra.

scholarly journals The supergiant O + O binary system HD 166734: a new study

2016 ◽  
Vol 12 (S329) ◽  
pp. 402-402 ◽  
Author(s):  
E. Gosset ◽  
L. Mahy ◽  
Y. Damerdji ◽  
C. Nitschelm ◽  
H. Sana ◽  
...  
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Radial Velocity ◽  
Velocity Curve ◽  
Physical Parameters ◽  
Radial Velocity Curve ◽  
X Ray ◽  
Orbital Parameters

AbstractWe present here a modern study of the radial velocity curve and of the photometric light curve of the very interesting supergiant O7.5If + O9I(f) binary system HD 166734. The physical parameters of the stars and the orbital parameters are carefully determined. We also perform the analysis of the observed X-ray light curve of this colliding-wind binary.

scholarly journals The analysis of SuperWASP photometric data for the overcontact binary QW Gem

2013 ◽  
pp. 47-51 ◽  
Author(s):  
A. Cséki
Keyword(s):  
Radial Velocity ◽  
Surface Brightness ◽  
Photometric Data ◽  
Physical Parameters ◽  
Eclipsing Binary ◽  
Photometric Observations ◽  
Modeling Code

The paper presents an analysis of photometric observations of the eclipsing binary QW Gem. The orbital and physical parameters of the system are derived using the modeling code by G. Djurasevic. Photometric observations are obtained from the SuperWASP public archive and the spectroscopic elements are adopted from a recently published radial velocity study. The results suggest that QW Gem is a binary in overcontact configuration, consisting of two stars of similar surface brightness but in different evolutionary stages.

scholarly journals TESS exoplanet candidates validated with HARPS archival data

2019 ◽  
Vol 622 ◽  
pp. L7 ◽  
Author(s):  
Trifon Trifonov ◽  
Jan Rybizki ◽  
Martin Kürster
Keyword(s):  
Light Curve ◽  
Radial Velocity ◽  
Planetary Systems ◽  
Archival Data ◽  
Velocity Analysis ◽  
Orbital Parameters ◽  
Mean Motion ◽  
Two Systems ◽  
Made In ◽  
Mean Motion Resonance

Aims. We aim at the discovery of new planetary systems by exploiting the transit light-curve results from observations made in TESS orbital observatory Sectors 1 and 2 and validating them with precise Doppler measurements obtained from archival HARPS data. Methods. Taking advantage of the reported TESS transit events around GJ 143 (TOI 186) and HD 23472 (TOI 174), we modeled their HARPS precise Doppler measurements and derived orbital parameters for these two systems. Results. For the GJ 143 system, TESS has reported only a single transit, and thus its period is unconstrained from photometry. Our radial velocity analysis of GJ 143 reveals the full Keplerian solution of the system, which is consistent with an eccentric planet with a mass almost twice that of Neptune and a period of Pb = 35.59−0.1+0.1 days. Our estimates of the GJ 143 b planet are fully consistent with the transit timing from TESS. We confirm the two-planet system around HD 23472, which according to our analysis is composed of two Neptune-mass planets in a possible 5:3 mean motion resonance.

IO Com: Is it a Non-secondary Minimum Star?

2014 ◽  
Vol 23 (1) ◽  
Author(s):  
Günay Taş ◽  
Serdar Evren
Keyword(s):  
Radial Velocity ◽  
Light Curves ◽  
Secondary Minimum ◽  
Eccentric Orbit ◽  
Eclipsing Binary ◽  
Orbital Parameters ◽  
Long Period ◽  
The Absolute

AbstractFour-color photometry of IO Com, a detached eclipsing binary with a long period (~53 d), was accomplished in 2004–2008. The absolute astrophysical and orbital parameters of the system were determined by the analysis of the light and radial velocity curves. No secondary minima in the light curves were detected. It was revealed that IO Com is the system with a highly eccentric orbit consisting of the components of mid-F spectral types. The calculated masses and radii of the primary and secondary components are: 1.32

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