The Massive Binary System RY Sct – New Solution of the Light Curves

Astrophysics ◽  
2020 ◽  
Vol 63 (2) ◽  
pp. 243-251
Author(s):  
N. Kochiashvili ◽  
I. Kochiashvili ◽  
R. Natsvlishvili ◽  
S. Beradze ◽  
M. Vardosanidze
Keyword(s):  
Binary System ◽  
Light Curves

scholarly journals New Data on the Eclipsing Binary V1848 Ori and Improved Orbital and Light Curve Solutions

2020 ◽  
Vol 29 (1) ◽  
pp. 72-80 ◽  
Author(s):  
Fatemeh Davoudi ◽  
Atila Poro ◽  
Fahri Alicavus ◽  
Afshin Halavati ◽  
Saeed Doostmohammadi ◽  
...  
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Mass Function ◽  
Light Curves ◽  
Complete Analysis ◽  
Physical Parameters ◽  
Mass Ratio ◽  
Third Body ◽  
Eclipsing Binary

AbstractNew observations of the eclipsing binary system V1848 Ori were carried out using the V filter resulting in a determination of new times of minima and new ephemeris were obtained. We presented the first complete analysis of the system’s orbital period behavior and analysis of O-C diagram done by the GA and MCMC approaches in OCFit code. The O-C diagram demonstrates a sinusoidal trend in the data; this trend suggests a cyclic change caused by the LITE effect with a period of 10.57 years and an amplitude of 7.182 minutes. It appears that there is a third body with mass function of f (m3) = 0.0058 M⊙ in this binary system. The light curves were analyzed using the Wilson-Devinney code to determine some geometrical and physical parameters of the system. These results show that V1848 Ori is a contact W UMa binary system with the mass ratio of q = 0.76 and a weak fillout factor of 5.8%. The O’Connell effect was not seen in the light curve and there is no need to add spot.

scholarly journals Variability of the Light Curves of the Close Binary GR Tauri

2002 ◽  
Vol 187 ◽  
pp. 337-338
Author(s):  
A. Yamasaki ◽  
M. Takeda ◽  
T. Yamauchi ◽  
G. Takada ◽  
S. Hattori
Keyword(s):  
Binary System ◽  
The State ◽  
Light Curves ◽  
Close Binary ◽  
Eclipsing Binary ◽  
Short Period ◽  
Contact Binary

AbstractVariability of the light curves of the short-period eclipsing binary system GR Tau (, almost-contact binary) is studied. It is found that GR Tau experienced both the state which is characterized by asymmetric light curves and the state characterized by symmetrical light curves.

scholarly journals δ Sct-Type Pulsators in Eclipsing Binary Systems: the Case of RZ Cas

2002 ◽  
Vol 185 ◽  
pp. 102-103
Author(s):  
E. Rodríguez ◽  
V. Costa ◽  
M.J. López-González ◽  
J.M. García ◽  
S.L. Kim ◽  
...  
Keyword(s):  
Binary System ◽  
Binary Systems ◽  
Hot Spot ◽  
Primary Component ◽  
Roche Lobe ◽  
Light Curves ◽  
Eclipsing Binary ◽  
Preliminary Results ◽  
The Impact

AbstractRZ Cas is an Algol-type eclipsing binary system where the primary component was recently discovered as a δ Set pulsator. A three-continent multisite photometric campaign was carried out during 1999. Preliminary results are reported here indicating a semi-detached system where the secondary fills its Roche lobe. The light curves also suggest a hot spot on the surface of the primary component as a consequence of the impact of the mass stream from the secondary. The pulsational behaviour can be well described with only one frequency.

scholarly journals UBV Photometry of the Massive Eclipsing Binary TT Aur

2001 ◽  
Vol 18 (2) ◽  
pp. 151-157 ◽  
Author(s):  
S. Özdemir ◽  
H. Ak ◽  
M. Tanriver ◽  
H. Gülseçen ◽  
S. Gülseçen ◽  
...  
Keyword(s):  
Binary System ◽  
Primary Component ◽  
Light Curves ◽  
National Observatory ◽  
Simultaneous Solution ◽  
Primary Minimum ◽  
Circumstellar Material ◽  
System Parameters ◽  
Ubv Photometry ◽  
Excess Absorption

AbstractUBV observations of the massive binary system TT Aur were carried out mainly at theTurkish National Observatory (TUG). These observations, together with IUE spectra and times of eclipse minima collected from the literature, were used to study the system parameters.Simultaneous solution of the light curves by the Wilson-Devinney code allows a semi-detached configuration with a slightly larger Roche-lobe filling secondary. This picture is supported by other evidence. The shoulders of the primary minimum suggest some excess absorption, in keeping with circumstellar material in the form of a disk-like structure around the primary component. The deeper primary minimum in the U filter may indicate a hotter region on the secondary-facing hemisphere of the primary.The period variation of the system can also be related to the possible existence of a third component in a circular orbit around the system.An alternative detached representation is also considered using optimal curve-fitting techniques. We appeal for further observations to help resolve some outstanding issues in this interesting massive binary.

scholarly journals Close Binary Star Observables: Modeling Innovations 2003-06

2006 ◽  
Vol 2 (S240) ◽  
pp. 188-197
Author(s):  
R. E. Wilson
Keyword(s):  
Parameter Estimation ◽  
Binary System ◽  
Binary Star ◽  
Thomson Scattering ◽  
Stellar Atmospheres ◽  
Light Curves ◽  
Close Binary ◽  
Line Profiles ◽  
Radiative Transfer Problem ◽  
Mass Ratios

AbstractInnovative work on close binary models in 2003-06 improved upon synthesized line spectra, line profiles, and polarimetry; developed new ways of parameter estimation; and increased solution effectiveness and efficiency. Recent applications demonstrate the analytic power of binary system line spectrum models that pre-date the triennium. X-ray binary line profiles and radial velocity curves were refined by solution of the radiative transfer problem with specific inclusion of X-irradiation. Model polarization curves were generated by Monte Carlo experiments with multiple Thomson scattering in thin and thick binary system disks. In the parameter estimation area, independent developments by two groups now allow measurement of ephemerides, apsidal motion, and third body parameters from whole light and velocity curves, to supplement the traditional way of eclipse timings. Although the new route to those parameters is not well known within the ephemeris community, there are accuracy advantages and the number of applications is increasing. Numerical solution experiments on photometric mass ratios have checked two views of their intuitive basis, and show that mass ratios are well determined where star radii and limiting lobe radii are both well determined, which is for semi-detached or over-contact binaries with total-annular eclipses. Solution efficiency and automatic operation is needed for processing of light curves from large surveys, and will also be valuable for preliminary solutions of individually observed binaries. Neural networks have mainly been used for classification, and now a neural network program reliably finds preliminary solutions for W UMa binaries. Archived model light curves and Fourier fitting also are being pursued for classification and for preliminary solutions. Light curves in physical units such as erg·sec−1·cm−3 now allow direct distance estimation by combining the absolute accuracy of model stellar atmospheres with the astrophysical detail of a physical close binary model, by means of rigorous scaling between surface emission and observable flux. A Temperature-distance (T-d) theorem specifies conditions under which temperatures of both stars and distance can be found from light and velocity curves.

scholarly journals An analysis of the light curves of the overcontact binary system V2388 Ophiuchi

2004 ◽  
Vol 417 (2) ◽  
pp. 725-730 ◽  
Author(s):  
K. Yakut ◽  
B. Kalomeni ◽  
C. İbanoğlu
Keyword(s):  
Binary System ◽  
Light Curves

scholarly journals Algol, Beta Lyrae, and W Serpentis: Some New Results for Three Well Studied Eclipsing Binaries

1989 ◽  
Vol 107 ◽  
pp. 35-49
Author(s):  
Edward F. Guinan
Keyword(s):  
Binary System ◽  
Physical Properties ◽  
Eclipsing Binaries ◽  
Light Curves ◽  
High Resolution Spectroscopy ◽  
Gas Flows ◽  
Photoelectric Photometry ◽  
Point Analysis ◽  
International Ultraviolet Explorer ◽  
Low Mass

AbstractThe properties of the eclipsing binaries Algol, Beta Lyrae, and W Serpentis are discussed and new results are presented. The physical properties of the components of Algol are now well determined. High resolution spectroscopy of the H-alpha feature by Richards et al. and by Gillet et al. and spectroscopy of the ultraviolet resonance lines with the International Ultraviolet Explorer satellite reveal hot gas around the BBV primary. Gas flows also have been detected apparently originating from the low mass, cooler secondary component and flowing toward the hotter star through the Lagrangian L1 point. Analysis of 6 years of multi-bandpass photoelectric photometry of Beta Lyrae indicates that systematic changes in light curves occur with a characteristic period of ≃275 ± 25 days. These changes may arise from pulsations of the B8II star or from changes in the geometry of the disk component. Hitherto unpublished u, v, b, y, and H-alpha index light curves of W Ser are presented and discussed. W Ser is a very complex binary system that undergoes complicated, large changes in its light curves. The physical properties of W Ser are only poorly known, but it probably contains one component at its Roche surface, rapidly transfering matter to a component which is embedded in a thick, opaque disk. In several respects, W Ser resembles an upscale version of a cataclysmic variable binary system.

Symbiotic Nova PU Vul - 33 Years of Observations

2012 ◽  
Vol 21 (1-2) ◽  
Author(s):  
S. Shugarov ◽  
D. Chochol ◽  
E. Kolotilov
Keyword(s):  
Binary System ◽  
Light Curves ◽  
Secondary Minimum ◽  
Pulsation Period ◽  
Primary Minimum ◽  
Cool Component ◽  
Period Analysis ◽  
Binary Orbit ◽  
Orbit Period

AbstractWe present UBVRI light curves of the symbiotic nova PU Vul after its outburst in 1978. Three observed eclipses of the hot component by the cool one were used to determine the ephemeris of the binary system as JD (Min I) = 2444550(15) + 4897(10) × E days. the 194-day shift of the secondary minimum from its expected positions in 2001 suggests the eccentricity of the binary orbit. Period analysis of the VRI photometry improved the pulsation period of the cool AGB variable in the system to P = 217.7 days. Pulsation of the cool component is detected only in the phases around the primary minimum, when the visible hemisphere of the AGB star is not influenced by the interaction with the hot component.

scholarly journals The newly discovered Be/X-ray binary Swift J004516.6–734703 in the SMC: witnessing the emergence of a circumstellar disc

2020 ◽  
Vol 499 (1) ◽  
pp. L41-L46
Author(s):  
J A Kennea ◽  
M J Coe ◽  
P A Evans ◽  
I M Monageng ◽  
L J Townsend ◽  
...  
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Light Curves ◽  
Type I ◽  
Pulsation Period ◽  
X Ray ◽  
Tidal Interaction ◽  
Long Period ◽  
Periodicity Analysis ◽  
Ir Light

ABSTRACT We report on the discovery of Swift J004516.6–734703, a Be/X-ray binary system by the Swift SMC Survey, S-CUBED. Swift J004516.6–734703, or SXP 146.6, was found to be exhibiting a bright (∼1037 erg s−1) X-ray outburst on 2020 June 18. The historical UV and IR light-curves from OGLE and Swift/UVOT showed that after a long period of steady brightness, it experienced a significant brightening beginning around 2019 March. This IR/UV rise is likely the signature of the formation of a circumstellar disc, confirmed by the presence of strong an H α line in SALT spectroscopy, that was not previously present. Periodicity analysis of the OGLE data reveals a plausible 426 d binary period, and in X-ray a pulsation period of 146.6 s is detected. The onset of X-ray emission from Swift J004516.6–734703 is likely the signature of a Type-I outburst from the first periastron passage of the neutron star companion through the newly formed circumstellar disc. We note that the formation of the circumstellar disc began at the predicted time of the previous periastron passage, suggesting its formation was spurred by tidal interaction with the neutron star.

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