scholarly journals V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System

2022 ◽  
Vol 924 (1) ◽  
pp. 30
Author(s):  
F.-X. Li ◽  
W.-P. Liao ◽  
S.-B. Qian ◽  
E. Fernández Lajús ◽  
J. Zhang ◽  
...  
Keyword(s):  
Mass Transfer ◽  
Triple System ◽  
Continuous Light ◽  
Close Binary ◽  
Massive Component ◽  
Cyclic Oscillation ◽  
Contact Binary ◽  
Period Decrease ◽  
First Time ◽  
Linear Period

Abstract V606 Centauri (V606 Cen) is an early B-type close binary with an orbital period of 1.4950935 days, and its complete light curves are very difficult to observe on the ground. By analyzing the continuous light curve obtained by TESS, we found that it is a marginal contact binary with a very low fill-out factor of about 2%. The O − C diagram of V606 Cen is constructed for the first time based on 118.8 yr of eclipse times. The O − C diagram has been found to show a downward parabolic change together with a cyclic oscillation with a semiamplitude of 0.0545 days and a period of 88.3 yr. The downward parabolic variation reveals a linear period decrease at a rate of dP/dt = −2.08 × 10−7 days yr−1 that can be explained by the mass transfer from the more massive component to the less massive one. Both the marginal contact configuration and the continuous period decrease suggest that V606 Cen is a newly formed contact binary via Case A mass transfer. The cyclic change in the O − C diagram can be explained by the light-travel time effect via the presence of a third body. The lowest mass of the tertiary companion is determined to be M 3 = 4.51 (±0.43) M ⊙ and the tertiary is orbiting around the central eclipsing binary in a nearly circular orbit (e = 0.33). All of the results indicate that V606 Cen is a newly formed massive contact binary in a hierarchical triple system.

scholarly journals Period Variation Study and Light Curve Analysis of the Eclipsing Binary GSC 02013-00288

2016 ◽  
Vol 1 (2) ◽  
pp. 321-334 ◽  
Author(s):  
N.S. Awadalla ◽  
M.A. Hanna ◽  
M.N. Ismail ◽  
I.A. Hassan ◽  
M.A. Elkhamisy
Keyword(s):  
Mass Transfer ◽  
Curve Analysis ◽  
Light Curves ◽  
Mass Ratio ◽  
Late Type ◽  
Light Curve Analysis ◽  
Orbital Inclination ◽  
Eclipsing Binary ◽  
Massive Component ◽  
Period Decrease

AbstractWe analyzed the first set of complete CCD light curves of the W UMa type eclipsing binary IK Boo in the BVRI bands by using the PHOEBE code and deduced its first photometric parameters with, mass ratio q = 0.648 and orbital inclination i = 63o. We have applied a spotted model due to the light curves asymmetry. The system shows a distinct O’Connell effect. The best solution fit to the light curves suggested the influence of star spot(s) on both components. Such presence of star spot(s) is common among the RS CVn and W UMa chromospheric active late type stars.We also present an analysis of mid–eclipse time measurements of IK Boo. The analysis indicates a period decrease rate dP/dt = −1.68 × 10−7d/yr, which can be interpreted in terms of mass transfer of rate 3.1 × 10−7M⊙/yr, from the more massive to the less massive component.

scholarly journals The Photometric Investigation of V921 Her Using the Lunar-Based Ultraviolet Telescope of Chang’e-3 Mission

2016 ◽  
Vol 2016 ◽  
pp. 1-6 ◽  
Author(s):  
Xiao Zhou ◽  
Sheng-Bang Qian ◽  
Jia Zhang ◽  
Lin-Jia Li ◽  
Qi-Shan Wang
Keyword(s):  
Binary System ◽  
Thermal Contact ◽  
Primary Star ◽  
Light Minimum ◽  
Evolutionary Scenario ◽  
Total Luminosity ◽  
Massive Component ◽  
Contact Binary ◽  
Photometric Investigation ◽  
First Time

The light curve of V921 Her in ultraviolet band observed by the Lunar-based Ultraviolet Telescope (LUT) is analyzed by the Wilson-Devinney code. Our solutions conclude that V921 Her is an early type marginal contact binary system with an additional close-in component. The binary system is under poor thermal contact with a temperature difference of nearly 700 K between the two components. The close-in component contributes about 19% of the total luminosity in the triple system. Combining the radial velocity study together with our photometric solutions, the mass of the primary star and secondary one is calculated to beM1=1.784  (±0.055)M⊙,M2=0.403  (±0.012)M⊙. The evolutionary scenario of V921 Her is discussed. All times of light minimum of V921 Her available in the bibliography are taken into account and theO-Ccurve is analyzed for the first time. The most probable fitting results are discussed in the paper, which also confirm the existence of a third component (P3=10.2year) around the binary system. The period of V921 Her is also undergoing a continuously rapid increase at a rate ofdP/dt=+2.79×10-7  day·year-1, which may be due to mass transfer from the less massive component to the more massive one.

Studies on the equatorial spot of G-type contact binary UV Lyn

2021 ◽  
Author(s):  
Jingjing Wang ◽  
Bin Zhang ◽  
Linqiao Jiang
Keyword(s):  
Magnetic Activity ◽  
The Past ◽  
Photometric Observations ◽  
Massive Component ◽  
Type Contact ◽  
Contact Binary ◽  
Periodic Trend ◽  
Short Time ◽  
First Time ◽  
Magnitude Difference

Abstract New CCD photometric observations of G-type contact binary UV Lyn were obtained in 2006 and 2020, when the light curves (LCs) show positive O'Connell effect and negative O'Connell effect, especially. From the previous studies, the LCs by other ground-based telescope are variable from 1973 to 2020, particularly the magnitude difference between the two maxima. These phenomena indicate that the component is active in the past 47 years. In addition, under the monitoring of the space telescope of Transiting Exoplant Survey Satellite (TESS) from January to March in 2020, we fortunately find the continuous variations of O'Connell effect in every circle for the first time. The analysis also shows that in a short time, the positive O'Connell effect has been transformed into the negative one, which proves that there are stronger magnetic activities on the surface of the component. By using the Wilson-Devinney code with a spot model, these photometric solutions confirm UV Lyn is a shallow W-subtype contact binary with a cool equatorial spot on the less massive component. The successive variability of O'Connell effect possibly result from one equatorial cool spot shifting gradually along with time. We also investigate its \emph{O-C} curve from these continuous LCs, there is not obvious variation in such short time. while, the O’Connell effect as the indicator of the magnetic activity are possibly undergoing a periodic trend of a period of nearly 38 days. Comparing \emph{O-C} curve, we could find there is not relation between the period variation and magnetic activity.

scholarly journals Response of low-mass main sequence stars to accretion

1981 ◽  
Vol 59 ◽  
pp. 401-403
Author(s):  
Masayuki Y. Fujimoto ◽  
Icko Iben ◽  
Stephen A. Becker
Keyword(s):  
Mass Transfer ◽  
Close Binary System ◽  
Close Binary ◽  
Mass Star ◽  
Main Sequence Stars ◽  
Massive Component ◽  
Low Mass ◽  
The Common ◽  
Rapid Mass ◽  
Number Of Authors

When the massive component in a close binary system evolves to fill its Roche lobe, mass transfer occurs and gas is accreted onto the companion star. Recently, the response of the unevolved secondary to accretion has been studied by a number of authors, but the emphasis has been on relatively massive stars which have a radiative envelope (Ulrich and Burger 1976; Flannery and Ulrich 1977; Kippenhalm and Meyer-Hofmeister 1977; Neo et al. 1977). The results show that the mass accepting star becomes overluminous and grows in radius until rapid mass transfer ultimately brings the two stars into contact. Such changes in the structure are caused by the steep increase in the specific entropy in the outermost layers and only a small amount of mass (about a tenth of the initial mass of the star) is accreted before contact is made. Thereafter, the expansion of the common envelope will lead to mass loss from the system. It is also found that, for a given accretion rate, the radial increase is much more conspicuous for a smaller mass star.

scholarly journals YZ Phoenicis: a very short period K-type contact binary with variation of the O’Connell effect and orbital period change

2019 ◽  
Vol 71 (4) ◽  
Author(s):  
Thawicharat Sarotsakulchai ◽  
Sheng-Bang Qian ◽  
Boonrucksar Soonthornthum ◽  
Xiao Zhou ◽  
Jia Zhang ◽  
...  
Keyword(s):  
Orbital Period ◽  
Hot Spot ◽  
Period Change ◽  
Third Body ◽  
Normal Contact ◽  
Short Period ◽  
Massive Component ◽  
Contact Binary ◽  
Period Decrease

Abstract YZ Phe is a very short-period contact binary (Sp. = K2 V) with an orbital period of 0.2347 d near the short period limit (0.22 d). We present the complete light curves which photometric data were obtained from the 60 cm telescope of PROMPT-8 at CTIO in Chile during 2016 June to October and 2017 August. The photometric solutions were determined by using the Wilson & Devinney code and the results reveal that YZ Phe is a W-subtype shallow contact binary ($f\sim 10\,$, q = 2.635, or 1/q = 0.379 for W subtype) with rotational motion of a large hot spot on the more massive component, showing a strong O’Connell effect with variation of maxima in photometric time series at period of 4.20 yr and stellar cycle at period of 1.28 yr. By compiling all available eclipse times, the result shows a long-term period decrease at a rate of dP/dt = −2.64(±0.02) × 10−8 d yr−1, superimposed on a cyclic variation (A3 = 0.0081 d and P3 = 40.76 yr). This variation cannot be explained by the Applegate mechanism. Thus, the cyclic change may be interpreted as the light-travel time effect via the presence of a cool third body. Based on photometric solutions, the third light was detected as $2\,$ of the total light in V and I bands. These results support the existence of a third body. The long-term period decrease can be explained by mass transfer from the more massive component ($M_2 \sim 0.74\, M_{\odot }$) to the less massive one ($M_1 \sim 0.28\, M_{\odot }$) or plus angular momentum loss (AML) via magnetic braking. With 1/q < 0.4 and long-term period decrease, all factors suggest that YZ Phe is on the AML-controlled state and its fill-out factor will increase, as well as the system evolving into a deeper normal contact binary.

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.

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.

scholarly journals Mass Transfer and Intrinsic Light Variability in the Contact Binary MT Cas

2019 ◽  
Vol 2019 ◽  
pp. 1-9
Author(s):  
Haifeng Dai ◽  
Huiyu Yuan ◽  
Yuangui Yang
Keyword(s):  
Mass Transfer ◽  
Dark Spot ◽  
Mass Ratio ◽  
Ccd Photometry ◽  
Contact Configuration ◽  
Massive Component ◽  
Contact Binary ◽  
Secular Increase ◽  
Weak Contact ◽  
Light Variability

First CCD photometry for the contact binary MT Cas is performed in 2013 in December. The spectral type of F8V is determined from the low-precision spectrum observed on 2018 Oct 22. With Wilson-Devinney code, the photometric solutions are deduced from VRc light curves (LCs) and AAVSO’s and ASAS-SN’s data, respectively. The results imply that MT Cas is a W-type weak-contact binary with a mass ratio of q=2.365(±0.005) and a fill-out factor of f=16.6(±1.2)%, respectively. The asymmetric LCs in 2013 are modeled by a dark spot on the more massive component. By analyzing the (O-C) curve, it is discovered that the orbital period may be undergoing a secular increase at a rate of dP/dt=1.12(±0.09)×10-8d  yr-1, which may result from mass transfer from the less massive component to the more massive one. With mass transferring, MT Cas may evolve into a broken-contact configuration as predicted by TRO theory.

scholarly journals Mass-transfer in close binary and their companions

2016 ◽  
Vol 728 ◽  
pp. 072020
Author(s):  
Wenping Liao ◽  
Shengbang Qian ◽  
Liying Zhu ◽  
Linjia Li
Keyword(s):  
Mass Transfer ◽  
Close Binary

MATHEMATICAL MODELING OF CONCRETE STRUCTURE CORROSION IN BIOLOGICALLY AGGRESSIVE ENVIRONMENTS

2021 ◽  
Vol 3 (102) ◽  
pp. 55-67
Author(s):  
VARVARA E. RUMYANTSEVA ◽  
SVETLANA A. LOGINOVA ◽  
NATALIA E. KARTSEVA
Keyword(s):  
Mathematical Modeling ◽  
Mathematical Model ◽  
Mass Transfer ◽  
Parabolic Type ◽  
Cement Concrete ◽  
Mass Conductivity ◽  
Kinetics And Dynamics ◽  
Biological Corrosion ◽  
First Time ◽  
Fourth Kind

In the aquatic environment, biocorrosion is an important factor affecting the reliability and durability of concrete structures. The destruction of cement concretes during biological corrosion is determined by the processes of mass transfer. The article presents the development of a calculated mathematical model of liquid corrosion in cement concrete, taking into account the biogenic factor. For the first time, a model of mass transfer in an unbounded two-layer plate is considered in the form of differential equations of parabolic type in partial derivatives with boundary conditions of the second kind at the interface between concrete and liquid and of the fourth kind at the interface between concrete and biofilm. The results of a numerical experiment are presented to study the influence of the coefficients of mass conductivity and mass transfer on the kinetics and dynamics of the process.

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