TZ Lyrae: an Algol-type Eclipsing Binary with Mass Transfer

2007 ◽  
Vol 7 (2) ◽  
pp. 258-264 ◽  
Author(s):  
Yuan-Gui Yang ◽  
Xin-Guo Yin
Keyword(s):  
Mass Transfer ◽  
Eclipsing Binary

scholarly journals LBT Discovery of a Yellow Supergiant Eclipsing Binary in the Dwarf Galaxy Holmberg IX

2007 ◽  
Vol 3 (S250) ◽  
pp. 333-338
Author(s):  
J. L. Prieto ◽  
K. Z. Stanek ◽  
C. S. Kochanek ◽  
D. R. Weisz
Keyword(s):  
Mass Transfer ◽  
Surface Temperature ◽  
Light Curve ◽  
Mass Loss ◽  
Dwarf Galaxy ◽  
Evolutionary Stage ◽  
Eclipsing Binary ◽  
Contact Binary ◽  
Yellow Supergiant

AbstractIn a variability survey of M81 using the Large Binocular Telescope we have discovered a peculiar eclipsing binary (MV ≃ −7.1) in the field of the dwarf galaxy Holmberg IX. It has a period of 271 days and the light curve is well-fit by an overcontact model in which both stars are overflowing their Roche lobes. It is composed of two yellow supergiants (V − I ≃ 1 mag, Teff = 4800 K), rather than the far more common red or blue supergiants. Such systems must be rare. While we failed to find any similar systems in the literature, we did, however note a second example. The SMC F0 supergiant R47 is a bright (MV ≃ −7.5) periodic variable whose All Sky Automated Survey (ASAS) light curve is well-fit as a contact binary with a 181 day period. We propose that these massive systems are the progenitors of supernovae like SN 2004et and SN 2006ov, which appeared to have yellow progenitors. The binary interactions (mass transfer, mass loss) limit the size of the supergiant to give it a higher surface temperature than an isolated star at the same core evolutionary stage.

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 Active Algol Binary KZ Pavonis

2001 ◽  
Vol 18 (2) ◽  
pp. 140-147 ◽  
Author(s):  
E. Budding ◽  
S. C. Marsden ◽  
O. B. Slee
Keyword(s):  
Mass Transfer ◽  
Radio Emission ◽  
Transfer Process ◽  
Mass Transfer Process ◽  
Photometric Data ◽  
Optical Data ◽  
Eclipsing Binary ◽  
Multi Wavelength ◽  
Low Levels ◽  
The University

AbstractThe Algol type eclipsing binary KZ Pav has been observed over one complete orbit (0.95 days) with theAustraliaTelescope CompactArray. Contemporaneous optical photometric data from the University of Southern Queensland’s Observatory at Mount Kent were also collected and have been included in this multi-wavelength study.Preliminary indications are that the low levels of emission observed share similarities to those of some RS CVn binaries. The optical data show phase-linked effects which can be related to the mass transfer process of Algols. The possibility that the radio emission may be related to this process is considered.

scholarly journals A tidally tilted sectoral dipole pulsation mode in the eclipsing binary TIC 63328020

2021 ◽  
Author(s):  
S A Rappaport ◽  
D W Kurtz ◽  
G Handler ◽  
D Jones ◽  
L A Nelson ◽  
...  
Keyword(s):  
Mass Transfer ◽  
Orbital Period ◽  
Mode Frequency ◽  
Prior History ◽  
Dipole Mode ◽  
Eclipsing Binary ◽  
Pulsation Mode ◽  
The Third ◽  
History Of ◽  
Binary Evolution

Abstract We report the discovery of the third tidally tilted pulsator, TIC 63328020. Observations with the TESS satellite reveal binary eclipses with an orbital period of 1.1057 d, and δ Scuti-type pulsations with a mode frequency of 21.09533 d−1. This pulsation exhibits a septuplet of orbital sidelobes as well as a harmonic quintuplet. Using the oblique pulsator model, the primary oscillation is identified as a sectoral dipole mode with l = 1, |m| = 1. We find the pulsating star to have M1 ≃ 2.5 M⊙, R1 ≃ 3 R⊙, and Teff, 1 ≃ 8000 K, while the secondary has M2 ≃ 1.1 M⊙, R2 ≃ 2 R⊙, and Teff, 2 ≃ 5600 K. Both stars appear to be close to filling their respective Roche lobes. The properties of this binary as well as the tidally tilted pulsations differ from the previous two tidally tilted pulsators, HD74423 and CO Cam, in important ways. We also study the prior history of this system with binary evolution models and conclude that extensive mass transfer has occurred from the current secondary to the primary.

scholarly journals KIC 8262223: A Post-mass Transfer Eclipsing Binary Consisting of a Delta Scuti Pulsator and a Helium White Dwarf Precursor

2017 ◽  
Vol 837 (2) ◽  
pp. 114 ◽  
Author(s):  
Zhao Guo ◽  
Douglas R. Gies ◽  
Rachel A. Matson ◽  
Antonio García Hernández ◽  
Zhanwen Han ◽  
...  
Keyword(s):  
Mass Transfer ◽  
White Dwarf ◽  
Eclipsing Binary ◽  
Delta Scuti

scholarly journals The Massive Eclipsing Binary RY Scuti

1982 ◽  
Vol 99 ◽  
pp. 383-386
Author(s):  
G. Giuricin ◽  
F. Mardirossian
Keyword(s):  
Mass Transfer ◽  
Binary Systems ◽  
Evolutionary Stage ◽  
Eclipsing Binary ◽  
Transfer Case

We have analyzed Ciatti et al's (1980) UBV lightcurves of the massive eclipsing binary RY Set. The BO primary, being considerably over-luminous and oversized for its mass, is certainly appreciably evolved. That this star is nearly filling its Robe lobe strongly supports the idea that it is undergoing a phase of mass transfer (case B), through Robe lobe overflow, towards its more massive secondary companion. In view of its properties, RY Set, which represents an uncommon evolutionary stage, is lively to evolve into a Wolf-Rayet binary systems.

scholarly journals V643 Orionis: A detached, evolved, post-mass-exchange eclipsing binary

2019 ◽  
Vol 624 ◽  
pp. A88 ◽  
Author(s):  
J. Andersen ◽  
G. Torres ◽  
J. V. Clausen
Keyword(s):  
Mass Transfer ◽  
Angular Momentum ◽  
Binary System ◽  
Mass Exchange ◽  
Light Curves ◽  
Sequence Evolution ◽  
Eclipsing Binary ◽  
Orbital Parameters ◽  
Stellar Properties ◽  
The Masses

Context. One of the greatest uncertainties in modelling the mass-exchange phases during the evolution of a binary system is the quantity of mass and angular momentum that has been lost from the system. To constrain this problem, a favourable, evolved, and detached real binary system is valuable as an example of the end result of this process. Aims. We study the 52-day post-mass-exchange eclipsing binary V643 Ori from complete uvby light curves and high-resolution spectra. V643 Ori is double-lined and shows total primary eclipses. The orbit is accurately circular and the rotation of the two stars is synchronised with the orbit, but the photometry from a single year (1993) shows signs of weak spot activity (0.02 mag) around the primary eclipse. Results. We determined accurate masses of 3.3 and 1.9 M⊙ from the spectroscopic orbit and solved the four light curves to determine radii of 16 and 21 R⊙, using the Wilson-Devinney photometric code. The rotational velocities from the cross-correlation profiles agree well with those computed from the known radii and orbital parameters. All observable parameters are thus very precisely determined, but the masses and radii of V643 Ori are incompatible with undisturbed post-main-sequence evolution. Conclusions. We have attempted to simulate the past evolutionary history of V643 Ori under both conservative and non-conservative Case B mass transfer scenarios. In the non-conservative case we varied the amounts of mass and angular momentum loss needed to arrive at the present masses in a circular 52-day orbit, keeping the two stars detached and synchronised as now observed, but without following the evolution of other stellar properties in any detail. Multiple possible solutions were found. Further attempts were made using both the BSE formalism and the binary MESA code in order to track stellar evolution more closely, and make use of the measured radii and temperatures as important additional constraints. Those efforts yielded no satisfactory solutions, possibly due to limitations in handling mass transfer in evolved stars such as these. We remain hopeful that future theoreticians can more fully model the system under realistic conditions.

scholarly journals KIC 10736223: An Algol-type Eclipsing Binary That Has Just Undergone the Rapid Mass-transfer Stage

2020 ◽  
Vol 895 (2) ◽  
pp. 136 ◽  
Author(s):  
Xinghao Chen ◽  
Xiaobin Zhang ◽  
Yan Li ◽  
Hailiang Chen ◽  
Changqing Luo ◽  
...  
Keyword(s):  
Mass Transfer ◽  
Eclipsing Binary ◽  
Rapid Mass ◽  
Transfer Stage

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.

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