scholarly journals Scanner observations of some close binary systems

1986 ◽  
Vol 118 ◽  
pp. 261-263
Author(s):  
D. J. Sullivan ◽  
M. Walkington ◽  
E. Budding
Keyword(s):  
Light Curve ◽  
Binary Systems ◽  
Light Curves ◽  
Close Binary ◽  
Eclipsing Binary ◽  
Close Binary Systems

Using our intermediate bandwidth photometric scanner, we have obtained light curve data at a range of spectral intervals for a number of close eclipsing binary systems. This paper reports briefly on the instrumentation system, the data obtained for two of the variables AE Phe and ε CrA, and a preliminary modelling of the light curves.

scholarly journals Explosion of White Dwarfs

1987 ◽  
Vol 93 ◽  
pp. 413-417
Author(s):  
R. Lopez ◽  
J. Isern ◽  
J. Labay ◽  
R. Canal
Keyword(s):  
Light Curve ◽  
White Dwarfs ◽  
Binary Systems ◽  
Light Curves ◽  
Close Binary ◽  
Classical Type ◽  
Type I ◽  
Close Binary Systems ◽  
Systems Studies

AbstractWe present models for Type I supernova light curves based on the explosion of partially solid white dwarfs in close binary systems. Studies of such explosions show that they leave bound remnants of different size. Our results reproduce quite well the maximun luminosities, the expansion velocities and the shape of the light curve. As the two basic papameters that govern the light curve, the ejected mass and the mass of 56Ni produced, are variable our models reproduce the slow and fast subclasses of “classical” Type I supernovae.

scholarly journals X-ray and UV emission of the ultrashort-period, low-mass eclipsing binary system BX Trianguli

2018 ◽  
Vol 619 ◽  
pp. A138
Author(s):  
V. Perdelwitz ◽  
S. Czesla ◽  
J. Robrade ◽  
T. Pribulla ◽  
J. H. M. M. Schmitt
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Binary Systems ◽  
Uv Light ◽  
Close Binary ◽  
Eclipsing Binary ◽  
X Ray ◽  
Uv Emission ◽  
Low Mass ◽  
Orbital Modulation

Context.Close binary systems provide an excellent tool for determining stellar parameters such as radii and masses with a high degree of precision. Due to the high rotational velocities, most of these systems exhibit strong signs of magnetic activity, postulated to be the underlying reason for radius inflation in many of the components. Aims.We extend the sample of low-mass binary systems with well-known X-ray properties. Methods.We analyze data from a singular XMM-Newton pointing of the close, low-mass eclipsing binary system BX Tri. The UV light curve was modeled with the eclipsing binary modeling tool PHOEBE and data acquired with the EPIC cameras was analyzed to search for hints of orbital modulation. Results.We find clear evidence of orbital modulation in the UV light curve and show that PHOEBE is fully capable of modeling data within this wavelength range. Comparison to a theoretical flux prediction based on PHOENIX models shows that the majority of UV emission is of photospheric origin. While the X-ray light curve does exhibit strong variations, the signal-to-noise ratio of the observation is insufficient for a clear detection of signs of orbital modulation. There is evidence of a Neupert-like correlation between UV and X-ray data.

scholarly journals Superoutbursts and Superhumps of SU UMa Stars

1988 ◽  
Vol 108 ◽  
pp. 238-239
Author(s):  
Yoji Osaki ◽  
Masahito Hirose
Keyword(s):  
Accretion Disk ◽  
Orbital Period ◽  
White Dwarf ◽  
Binary Systems ◽  
Roche Lobe ◽  
Light Curves ◽  
Close Binary ◽  
Dwarf Novae ◽  
Dwarf Nova ◽  
Close Binary Systems

SU UMa stars are one of subclasses of dwarf novae. Dwarf novae are semi-detached close binary systems in which a Roche-lobe filling red dwarf secondary loses matter and the white dwarf primary accretes it through the accretion disk. The main characteristics of SU UMa subclass is that they show two kinds of outbursts: normal outbursts and superoutbursts. In addition to the more frequent narrow outbursts of normal dwarf nova, SU UMa stars exhibit “superoutbursts”, in which stars reach about 1 magnitude brighter and stay longer than in normal outburst. Careful photometric studies during superoutburst have almost always revealed the “superhumps”: periodic humps in light curves with a period very close to the orbital period of the system. However, the most curious of all is that this superhump period is not exactly equal to the orbital period, but it is always longer by a few percent than the orbital period.

scholarly journals Remarks on the Complicated Close Binary Systems RT Lacertae, CG Cygni, and RW Coronae Borealis

1980 ◽  
Vol 88 ◽  
pp. 419-422
Author(s):  
E. F. Milone ◽  
S. A. Naftilan
Keyword(s):  
Light Curve ◽  
Binary Systems ◽  
Circumstellar Matter ◽  
Contact System ◽  
Close Binary ◽  
Close Binary Systems ◽  
Period Variability

The three systems differ in period, scale and degree of contact: RW Com is a contact system, RT Lac is semi-detached and CG Cyg is a detached system. Yet they share the properties of a variable asymmetric light curve in the UBV, Ca II H and K emission, apparent infrared excesses, and period variability. If it may be argued that this ensemble of symptoms has similar origins in the different systems, then our intensive studies of these three binaries may have implications for the nature of all systems showing the RS CVn properties. We feel that the evidence points to the presence of circumstellar matter in the three binaries. We pose the questions: does this material create the photometric pecularities, is it incidental to them or does it arise from some other light-curve perturbing source?

scholarly journals IUE Ultraviolet Spectra of the Interacting Binary U Cephei

1980 ◽  
Vol 88 ◽  
pp. 237-241
Author(s):  
Yoji Kondo ◽  
George E. McCluskey ◽  
Robert E. Stencel
Keyword(s):  
High Resolution ◽  
Ultraviolet Light ◽  
Stellar Evolution ◽  
Binary Systems ◽  
Light Curves ◽  
Close Binary ◽  
Eclipsing Binary ◽  
Ultraviolet Spectra ◽  
International Ultraviolet Explorer ◽  
Far Ultraviolet

The eclipsing binary U Cephei has proven to be of great interest in the study of stellar evolution in close binary systems. Batten (1974), Hall and Walter (1974), Rhombs and Fix (1976), Markworth (1977), and Olson (1978), among others, have recently reported on their intensive ground based studies of U Cephei. Kondo, McCluskey and Wu (1978) have investigated the ultraviolet light curves of U Cephei obtained with Astronomical Netherlands Satellite (ANS). Kondo, McCluskey and Stencel (1979) have discussed the International Ultraviolet Explorer (IUE) spectra of U Cephei. This paper discusses results incorporating additional IUE high resolution spectra of U Cephei obtained in both far-ultraviolet and mid-ultraviolet spectral regions.

scholarly journals Synthetic Light Curve Analysis of the Close Binary Systems BX Andromedae and RR Leporis

1989 ◽  
Vol 107 ◽  
pp. 359-360
Author(s):  
R.G. Samec ◽  
R.E. Fuller ◽  
R. H. Kaitchuck ◽  
B. B. Bookmyer ◽  
D. R. Faulkner
Keyword(s):  
Light Curve ◽  
Binary Systems ◽  
Thermal Relaxation ◽  
Curve Analysis ◽  
Light Curves ◽  
Close Binary ◽  
Comparison Star ◽  
Short Time Scale ◽  
Light Curve Analysis ◽  
Short Period

AbstractUnpublished photoelectric observations of the systems BX And and RR Lep were subjected to light curve analysis using the Wilson-Devinney Code.The short-period eclipsing binary system BX And was observed on five nights in 1976 at the Morgan-Monroe station of the Goethe Link Observatory of Indiana University. The observations covering the eclipse portions of the light curves yielded four times of minimum light. A period study covering 89 years of observations confirms that a major period change took place about 1950. The system is suspected of being quite active on a short time scale. Standard magnitudes were derived for BX And and for the comparison star. The corrected color indices indicate that BX And and the comparison star BD+39° 476 are in the spectral range of F3-F5. The light curves, defined by 1092 observations in B, 1097 in V and 971 in the U filter are symmetric. The difference in the eclipse depths are quite large averaging 0.m46. A distinct de-reddening of the light curves occurs during the secondary eclipse. The first synthetic light curve solutions of the system were obtained. The solution of BX And indicates that the system consists of an F-type primary and a K-type secondary component in a state of shallow contact. This result is supported by the location of BX And on the Eggen period-color diagram for contact binaries. The large mass ratio, temperature disparity and period increase are found to be consistent with an early contact phase of thermal relaxation oscillations.

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.

Synthetic light curve analysis of the close binary systems BX Andromedae and RR Leporis

1989 ◽  
Vol 50 (1-2) ◽  
pp. 359-360
Author(s):  
R.G. Samec ◽  
R.E. Fuller ◽  
R.H. Kaitchuck ◽  
B.B. Bookmyer ◽  
D.R. Faulkner
Keyword(s):  
Light Curve ◽  
Binary Systems ◽  
Curve Analysis ◽  
Close Binary ◽  
Light Curve Analysis ◽  
Close Binary Systems

Synthetic Light Curve Analysis of the Close Binary Systems BX Andromedae and RR Leporis

Algols ◽  
1989 ◽  
pp. 359-360
Author(s):  
R. G. Samec ◽  
R. E. Fuller ◽  
R. H. Kaitchuck ◽  
B. B. Bookmyer ◽  
D. R. Faulkner
Keyword(s):  
Light Curve ◽  
Binary Systems ◽  
Curve Analysis ◽  
Close Binary ◽  
Light Curve Analysis ◽  
Close Binary Systems

scholarly journals The BANANA Survey: Spin-Orbit Alignment in Binary Stars

2011 ◽  
Vol 7 (S282) ◽  
pp. 397-398 ◽  
Author(s):  
Simon Albrecht ◽  
J. N. Winn ◽  
D. C. Fabrycky ◽  
G. Torres ◽  
J. Setiawan
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Planet Formation ◽  
Close Binary ◽  
Spin Orbit ◽  
Eclipsing Binary ◽  
System Parameters ◽  
Close Binary Systems ◽  
Orbital Axis

AbstractBinaries are not always neatly aligned. Previous observations of the DI Herculis system showed that the spin axes of both stars are highly inclined with respect to one another and the orbital axis. Here, we report on our ongoing survey to measure relative orientations of spin-axes in a number of eclipsing binary systems.These observations will hopefully lead to new insights into star and planet formation, as different formation scenarios predict different degrees of alignment and different dependencies on the system parameters. Measurements of spin-orbit angles in close binary systems will also create a basis for comparison for similar measurements involving close-in planets.

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