scholarly journals AN ASTROMETRIC AND PHOTOMETRIC STUDY OF THE INTERMEDIATE-AGE OPEN CLUSTER NGC 2158 AND ITS ECLIPSING BINARY [NBN2015]78

2020 ◽  
Vol 56 (2) ◽  
pp. 245-257
Author(s):  
A. E. Abdelaziz ◽  
Y. H. M. Hendy ◽  
A. Shokry ◽  
S. M. Saad ◽  
F. Y. Kamal ◽  
...  
Keyword(s):  
Open Cluster ◽  
Distance Modulus ◽  
Mass Ratio ◽  
Photometric Analysis ◽  
Eclipsing Binary ◽  
Color Excess ◽  
Contact Binary ◽  
Cluster Age ◽  
Gaia Dr2 ◽  
Intrinsic Distance

We present a photometric and astrometric analysis of the NGC 2158 cluster using Gaia DR2 and 2MASS data. The cluster age, color excess, intrinsic distance modulus and distance are calculated to be t = 2.240 ± 0.260 Gyr, E(B − V) = 0.420 ± 0.050 mag, (m − M)⨀ = 12.540 ± 0.130 mag and d⨀ = 3224 ± 200 pc respectively. The photometric analysis and light curve modelling of the proposed eclipsing binary member [NBN2015]78 is performed using the latest version of the Wilson-Devinney (W-D) code. The solutions show that the system is an over-contact binary with a secondary component filling its Roche lobe, with a mass ratio q = 0.262. The primary and the secondary components of the system consist of two late spectral types K1 and K2 respectively. The membership of [NBN2015]78 is discussed using two independent methods, and we find that [NBN2015]78 is an interloper and not a member of NGC 2158.

scholarly journals STUDY OF AN INTERMEDIATE AGE OPEN CLUSTER IC 1434 USING GROUND-BASED IMAGING AND GAIA DR2 ASTROMETRY

2021 ◽  
Vol 57 (2) ◽  
pp. 381-389
Author(s):  
Y. H. M. Hendy ◽  
D. Bisht
Keyword(s):  
Radial Distribution ◽  
Proper Motion ◽  
Open Cluster ◽  
Membership Probability ◽  
Kinematical Analysis ◽  
The Mean ◽  
First Time ◽  
Right Ascension ◽  
Cluster Age ◽  
Gaia Dr2

We present a detailed photometric and kinematical analysis of the poorly studied open cluster IC 1434 using CCD VRI, APASS, and Gaia DR2 database for the first time. By determining the membership probability of stars we identify the 238 most probable members with a probability higher than 60%; by using proper motion and parallax data as taken from the Gaia DR2 catalog. The mean proper motion of the cluster is obtained as μx=−3.89±0.19 and μy=−3.34±0.19 mas yr−1 in both the directions of right ascension and declination. The radial distribution of member stars provides the cluster extent as 7.6 arcmin. We estimate the interstellar reddening E(B−V) as 0.34 mag using the transformation equations from the literature. We obtain the values of cluster age and distance as 631±73 Myr and 3.2±0.1 kpc.

scholarly journals Spectroscopic Observations of the Early-Type Contact Binary AW Lacertae

1989 ◽  
Vol 107 ◽  
pp. 354-354
Author(s):  
Y. Nakamura ◽  
A. Okazaki ◽  
J. Katahira
Keyword(s):  
Spectral Type ◽  
Variable Stars ◽  
Radial Velocities ◽  
Early Type ◽  
Mass Ratio ◽  
Photometric Analysis ◽  
Spectroscopic Observations ◽  
Type Contact ◽  
Contact Binary ◽  
Photometric Solution

Abstract.Spectroscopic observations were performed of the early-type contact binary AW Lac with an image-intensified coude spectrograph of 1.9−m telescope at the Okayama Astro-physical Observatory. A total of twenty-two spectra covering blue region with a dispersion of 16 Amm−1 have been secured on Kodak IIa-O baked plates. In every spectra sharp interstellar Call H,K lines are clearly seen. The spectral type of AW Lac has been estimated as early B, which substantially confirms the one adopted in the photometric analysis by Jiang et al. (1983) and is diffrent from A0 listed in General Catalogue of Variable Stars (Kholopov et al. 1985). Contrary to the suggestion by the photometric solution of Jiang et al., no definite secondary lines could be separated, though some indications of light contamination due to the secondary component are surely observed. This would imply that the light ratio of the components should be somewhat smaller than that derived by photometric analysis. No emission features appeared either. The measurement of radial velocities of the primary component for the orbital elements was made for twenty spectra by a conventional method. It was difficult to measure the radial velocities because the lines are quite broadened and deformed. Hence the measured values for the radial velocities should be regarded as rather preliminary. The derived spectroscopic elements, combined with the photometric data, give the absolute dimensions of the system for each assumed mass ratio q. For q = 1, being the adopted photometric solution by Jiang et al., we obtain too small value for the primary’s mass, comparing with its spectral type. For the mass ratio as small as q = 0.6, we can obtain a reasonable value for the mass of the primary. However, in order to get more definite conclusion the cross-correlation method would be more appropriate for the spectroscopic analysis of this system.

scholarly journals UBVRI Photometric Analysis of the Solar-Type Eclipsing Binary TYC 3034-299-1

2012 ◽  
Vol 2012 ◽  
pp. 1-11
Author(s):  
Ronald G. Samec ◽  
Adam Jaso ◽  
Jesse White ◽  
Danny R. Faulkner ◽  
Nicholas Blum ◽  
...  
Keyword(s):  
Light Curve ◽  
Massive Star ◽  
Light Curves ◽  
Dark Spot ◽  
Mass Ratio ◽  
Photometric Analysis ◽  
Contact Binary ◽  
Solar Type ◽  
Curve Solution ◽  
Light Curve Solution

TYC 3034-0299-1 (CVn) is a magnetically active, contact binary, ROTSE variable. UBVRcIc light curves are presented along with a period study and a simultaneous UBVRI light curve solution. Our light curves show eclipse amplitudes of 0.72 and 0.62 mags (V) in the primary and secondary eclipses. Modeled results include a dark spot region, found at longitude 51°, a 24% Roche lobe fill-out, and a mass ratio of 0.48. A total eclipse is found to occur in the secondary eclipse making TYC 3034-0299-1 a W-type (less massive star is hotter) W UMa variable.

Photometric analysis of a blue straggler eclipsing binary in the old open cluster NGC 2141

2012 ◽  
Vol 55 (8) ◽  
pp. 1500-1504 ◽  
Author(s):  
YangPing Luo ◽  
Bo Wang ◽  
HaiLiang Chen ◽  
XiaoBin Zhang ◽  
ZhanWen Han
Keyword(s):  
Open Cluster ◽  
Photometric Analysis ◽  
Eclipsing Binary ◽  
Blue Straggler

scholarly journals V752 Cen - A triple-lined spectroscopic contact binary with sudden and continuous period changes

2019 ◽  
Author(s):  
X Zhou ◽  
B Soonthornthum ◽  
S-B Qian ◽  
E Fernández Lajús
Keyword(s):  
Mass Transfer ◽  
Light Curves ◽  
Period Variation ◽  
Mass Ratio ◽  
Eclipsing Binary ◽  
Two Component ◽  
Massive Component ◽  
Contact Binary ◽  
The Absolute ◽  
Year 2000

Abstract V752 Cen is a triple-lined spectroscopic contact binary. Its multi-colour light curves were obtained in the years 1971 and 2018, independently. Photometric analyses reveal that the two sets of light curves produce almost consistent results. It contains a W-subtype totally eclipsing binary, and its mass ratio and fill-out factor are q = 3.35(1) and $f = 29(2)\, {{\ \rm per\ cent}}$. The absolute elements of its two component stars were determined to be M1 = 0.39(2)M⊙, M2 = 1.31(7)M⊙, R1 = 0.77(1)R⊙, R2 = 1.30(2)R⊙, L1 = 0.75(3)L⊙ and L2 = 2.00(7)L⊙. The period of V752 Cen is 0.37023198 day. The 0.37-d period remained constant from its first measurement in 1971 until the year 2000. However, it changed suddenly around the year 2000 and has been increasing continuously at a rate of dP/dt = +5.05 × 10−7day · year−1 since then, which can be explained by mass transfer from the less massive component star to the more massive one with a rate of $\frac{dM_{2}}{dt}=2.52\times {10^{-7}}M_\odot /year$. The period variation of V752 Cen over the 48 years in which the period has been monitored is really unusual, and is potentially related to effects from the possible presence of a nearby third star or of a pair of stars in a second binary.

scholarly journals ZZ Piscis Austrinus (ZZ PsA): a bright red nova progenitor and the instability mass ratio of contact binary stars

2020 ◽  
Vol 501 (1) ◽  
pp. 229-235
Author(s):  
Surjit S Wadhwa ◽  
Ain De Horta ◽  
Miroslav D Filipović ◽  
N F H Tothill ◽  
Bojan Arbutina ◽  
...  
Keyword(s):  
Binary System ◽  
Binary Stars ◽  
Current Status ◽  
Mass Ratio ◽  
Photometric Analysis ◽  
Spectral Class ◽  
Contact Binary Stars ◽  
Contact Binary ◽  
Low Mass ◽  
Low Mass Ratio

ABSTRACT ZZ Piscis Austrinus (ZZ PsA) is a neglected bright southern contact binary system with maximum V magnitude of 9.26. We present the first multiband photometric analysis and find the system to be in deep contact (>95 per cent) with an extremely low mass ratio of 0.078. The primary has a mass of 1.213 M⊙ in keeping with its reported spectral class of F6. In order to determine if ZZ PsA is a merger candidate, we outline the current status regarding the instability mass ratio and develop new relationship linking the mass of the primary to the instability mass ratio of the system and the degree of contact. We find that ZZ PsA along with two other examples from the literature to be merger candidates while an additional three require further observations to be confirmed as potential merger candidates.

Distribution of physical parameters for 380 contact binaries in the Kepler field

2020 ◽  
Vol 72 (6) ◽  
Author(s):  
Xu-Zhi Li ◽  
Liang Liu ◽  
Li-Ying Zhu
Keyword(s):  
Binary Systems ◽  
Large Mass ◽  
Eclipsing Binaries ◽  
Physical Parameters ◽  
Mass Ratio ◽  
Eclipsing Binary ◽  
Contact Binaries ◽  
Contact Binary ◽  
Low Mass ◽  
Low Mass Ratio

Abstract We present the physical parameters (p, T, q, i, f) of 380 Kepler contact binary systems (hereafter called CBs). A statistical study on the CBs is carried out based on a Kepler photometric database. Our samples were selected from the Kepler Eclipsing Binary Catalogue of EW-type eclipsing binaries with periods around 0.2–1 d and amplitudes greater than $5\%$. The physical parameters were obtained by fitting the Kepler light curves with the Wilson–Devinney eclipsing binary modeling program. Our sample of CBs contains 160 A-type and 220 W-type CBs. The fill-out factor distribution indicated that CBs generally have shallow fill-out; the proportion of CBs with fill-out factors less than $30\%$ is around $70\%$, which may be related to the formation and evolution of the CBs. The period–temperature relationship of CBs is consistent with previous studies, which is the well-known period–color relationship. The distribution between mass ratio and fill-out factor can provide some information for studying the deep, low-mass ratio contact binaries and CBs which have a large mass ratio. The mass–radius diagram shows that there is a similar linear relationship between the primary and secondary stars while the primary stars are located almost on the ZAMS line; this could be related to the internal nuclear reaction within the primary and secondary stars.

scholarly journals Analysis of the Open Cluster NGC 2281

Galaxies ◽  
2021 ◽  
Vol 9 (1) ◽  
pp. 7
Author(s):  
Dirk Terrell ◽  
John Gross ◽  
Walter R. Cooney
Keyword(s):  
Variable Star ◽  
American Association ◽  
Open Cluster ◽  
Standard System ◽  
Proper Motions ◽  
Eclipsing Binary ◽  
Photometric Observations ◽  
Sky Survey ◽  
Gaia Dr2

BV observations of an approximately 68′×48′ field centered on the open cluster NGC 2281 and covering more than 400 nights from 2013 to 2018 are presented. The photometric observations were transformed to the standard system using standards from the American Association of Variable Star Observers Photometric All-sky Survey (APASS) DR10 and analyzed with Gaia DR2 parallaxes and proper motions to determine the distance, age, and metallicity of the cluster. The discovery of an eclipsing binary in the field is discussed.

The first photometric analysis of two low mass ratio totally eclipsing contact binaries: TIC 393943031 and TIC 89428764

2021 ◽  
Author(s):  
Yanke Tang ◽  
Yani Guo ◽  
Kai Li ◽  
Ning Gai ◽  
Zhikai Li
Keyword(s):  
Mass Transfer ◽  
Primary Component ◽  
Mass Ratio ◽  
Photometric Analysis ◽  
Angular Momenta ◽  
Contact Binaries ◽  
Contact Binary ◽  
Low Mass ◽  
Low Mass Ratio ◽  
First Time

Abstract PhotometricanalysisofthecontactbinariesTIC393943031andTIC89428764was carried out usingTESS and SuperWASP data for the first time. Using Wilson-Devinneycode, we have discovered TIC 393943031 is a low-mass-ratio deep contact binary with a fillout factor of 50.9(±1)% and a mass ratio of q = 0.163 ± 0.001. TIC 89428764 is a medium and low-mass-ratio contact binary with a fillout factor of 34.5(±1)% and a mass ratio of q = 0.147±0.001. Furthermore, the period study reveals both the stars exhibit continuously increasing periods, the increasing rate is 4.21×10−7day ·year−1for TIC 393943031while 6.36 × 10−7day · year−1for TIC 89428764. The possible reason is mass transfer from the secondary component to the primary component for both the stars. Meanwhile, we discussed their evolutionary phases and orbital angular momenta.

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