Photometric Observations of the Eclipsing Binary LT Herculis

1974 ◽  
Vol 86 ◽  
pp. 203 ◽  
Author(s):  
E. G. Ebbighausen ◽  
Gerald Penegor
Keyword(s):  
Eclipsing Binary ◽  
Photometric Observations

scholarly journals Towards a fully automated eclipsing binary solver for Gaia

2008 ◽  
Vol 4 (S253) ◽  
pp. 402-403
Author(s):  
Brandon Tingley ◽  
Gilles Sadowski ◽  
Christos Siopis
Keyword(s):  
Radial Velocity ◽  
High Precision ◽  
Eclipsing Binaries ◽  
Physical Parameters ◽  
Graphical Interface ◽  
Velocity Measurements ◽  
New Approach ◽  
Eclipsing Binary ◽  
Photometric Observations

AbstractGaia, an ESA cornerstone mission, will obtain of the order of 100 high-precision photometric observations and lower precision radial velocity measurements over five years for around a billion stars – several hundred thousand of which will be eclipsing binaries. In order to extract the characteristics of these systems, a fully automated code must be available. During the process of this development, two tools that may be of use to the transit community have emerged: a very fast, simple, detached eclipsing binary simulator/solver based on a new approach and an interacting eclipsing binary simulator with most of the features of the Wilson-Devinney and Nightfall codes, but fully documented and written in easy-to-follow and highly portable Java. Currently undergoing development and testing, this code includes an intuitive graphical interface and an optimizer for the estimation of the physical parameters of the system.

scholarly journals Spectral and photometric analysis of the eclipsing binary ε Aurigae prior to and during the 2009-2011 eclipse

2017 ◽  
Author(s):  
P. Chadima ◽  
M. Šlechta ◽  
P. Škoda ◽  
P. Harmanec ◽  
P. D. Bennett ◽  
...  
Keyword(s):  
Spectral Lines ◽  
Primary Star ◽  
Photometric Variability ◽  
Eclipsing Binary ◽  
Photometric Observations ◽  
Plausible Values ◽  
Ubv Photometry ◽  
Dominant Period ◽  
First Contact ◽  
Rule Out

A series of 353 red electronic spectra (from three observatories, mostly from 6300 to 6700 )A obtained between 1994 and 2010, and of 171 UBV photometric observations (from two observatories) of the 2010 eclipse, were analyzed in an effort to better understand ε Aur, the well-known, but still enigmatic eclipsing binary with the longest known orbital period (~27 yrs). The main results follow. (1) We attempted to recover a spectrum of the companion by disentangling the observed spectra of the ε Aur binary failed, but we were able to disentangle the spectrum of telluric lines and obtain a mean spectrum of the F-type primary star. The latter was then compared to a grid of synthetic spectra for a number of plausible values of Teff and log g, but a reasonably good match was not found. However, we conclude that the observed spectrum is that of a low gravity star. (2) We examined changes in the complex Halpha line profiles over the past 16 years, with particular emphasis on the 2009-2011 eclipse period, by subtracting a mean out-of-eclipse Halpha profile (appropriately shifted in radial velocity) from the observed spectra. We find that the dark disk around the unseen companion has an extended "atmosphere" that manifests itself via blueshifted and redshifted Halpha "shell" absorptions seen projected against the F star. Significantly, the Halpha shell line first appeared three years before first contact of the optical eclipse when the system was not far past maximum separation. (3) Analyses of radial velocities and central intensities of several strong, unblended spectral lines, as well as UBV photometry, demonstrated that these observables showed apparent multiperiodic variability during eclipse. The dominant period of 66.21d was common to all the observables, but with different phase shifts between these variables. This result strongly supports our earlier suggestion that the photometric variability seen during eclipse is intrinsic to the F star, and therefore, the idea of a central brightening due to a hole in the disk should be abandoned. Although variability on similar timescales is also seen in the spectrum and in photometry out of eclipse, we were unable to find a coherent periodicity in these data. Nevertheless, theseresults appear to rule out regular stellar pulsations as the cause of this variability. Based on spectra obtained at the Dominion Astrophysical Observatory, Ondrejov Observatory and Castanet-Tolosan Observatory and on UBV photometry gathered at the Hvar Observatory and Hopkins Phoenix Observatory.Tables 1 and 2 are only available at the CDS via anonymous ftp to cdarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/530/A146

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 V772 Cas: an ellipsoidal HgMn star in an eclipsing binary

2020 ◽  
Vol 500 (2) ◽  
pp. 2577-2589
Author(s):  
O Kochukhov ◽  
C Johnston ◽  
J Labadie-Bartz ◽  
S Shetye ◽  
T A Ryabchikova ◽  
...  
Keyword(s):  
Brightness Variation ◽  
Primary Component ◽  
Eclipsing Binaries ◽  
High Resolution Spectroscopy ◽  
Eclipsing Binary ◽  
Fundamental Parameters ◽  
Chemically Peculiar ◽  
Photometric Observations ◽  
Peculiar Stars ◽  
Chemically Peculiar Stars

ABSTRACT The late B-type star V772 Cas (HD 10260) was previously suspected to be a rare example of a magnetic chemically peculiar star in an eclipsing binary system. Photometric observations of this star obtained by the TESS satellite show clear eclipses with a period of 5.0137 d accompanied by a significant out-of-eclipse variation with the same period. High-resolution spectroscopy reveals V772 Cas to be an SB1 system, with the primary component rotating about a factor two slower than the orbital period and showing chemical peculiarities typical of non-magnetic HgMn chemically peculiar stars. This is only the third eclipsing HgMn star known and, owing to its brightness, is one of the very few eclipsing binaries with chemically peculiar components accessible to detailed follow-up studies. Taking advantage of the photometric and spectroscopic observations available for V772 Cas, we performed modelling of this system with the phoebe code. This analysis provided fundamental parameters of the components and demonstrated that the out-of-eclipse brightness variation is explained by the ellipsoidal shape of the evolved, asynchronously rotating primary. This is the first HgMn star for which such variability has been definitively identified.

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 NEW CCD TIMES OF MINIMA OF ECCENTRIC ECLIPSING BINARY SYSTEMS IN 2017-2019

2020 ◽  
pp. 1-16
Author(s):  
M.-J. Jeong ◽  
C.-H. Kim ◽  
M.-H. Song ◽  
E.-C. Sung ◽  
J.-H. Park ◽  
...  
Keyword(s):  
Binary Systems ◽  
Astronomical Observatory ◽  
Republic Of Korea ◽  
Eclipsing Binary ◽  
Photometric Observations

We present 88 times of minima for 56 eccentric eclipsing binary systems determined from photometric observations at the Sobaeksan Optical Astronomical Observatory (SOAO) in Republic of Korea from February 2017 to December 2019.

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