scholarly journals Marginally low mass ratio close binary system V1191 Cyg

New Astronomy ◽  
2012 ◽  
Vol 17 (1) ◽  
pp. 46-49 ◽  
Author(s):  
B. Ulaş ◽  
B. Kalomeni ◽  
V. Keskin ◽  
O. Köse ◽  
K. Yakut
Keyword(s):  
Binary System ◽  
Close Binary System ◽  
Close Binary ◽  
Mass Ratio ◽  
Low Mass ◽  
Low Mass Ratio

scholarly journals ON THE CHROMOSPHERIC ACTIVITY NATURE OF A LOW-MASS CLOSE BINARY: KIC 12004834

2019 ◽  
Vol 55 (1) ◽  
pp. 73-92
Author(s):  
E. Yoldaş ◽  
H. A. Dal
Keyword(s):  
Binary System ◽  
Close Binary System ◽  
Close Binary ◽  
Flare Activity ◽  
Mass Ratio ◽  
Orbital Inclination ◽  
Chromospheric Activity ◽  
Low Mass ◽  
High Level ◽  
Flare Frequency

We study the nature of the chromospheric activity of an eclipsing binary KIC 12004834, using Kepler data. We analyse the light curve of the system, the sinusoidal variations at out-of-eclipses and detected flare events. The secondary component’s temperature is found to be 4001±11 K, the mass ratio is 0.743±0.001, and the orbital inclination is 75◦.89±0◦.03. The analysis indicates a stellar spot effect on the variation. Moreover, the OPEA model has been derived over 149 flares. The saturation level called Plateau value, is found to be 2.093±0.236 s. The flare number per hour (known as flare frequency N1) is found to be 0.06644 h−1, while the flare-equivalent duration per hour (known as flare frequency N2) is found to be 0.59 second/hour. According to these results, KIC 12004834 is a very low-mass close binary system with high level of flare activity.

ASAS J083241+2332.4: A NEW EXTREME LOW MASS RATIO OVERCONTACT BINARY SYSTEM

2016 ◽  
Vol 151 (3) ◽  
pp. 69 ◽  
Author(s):  
K. Sriram ◽  
S. Malu ◽  
C. S. Choi ◽  
P. Vivekananda Rao
Keyword(s):  
Binary System ◽  
Mass Ratio ◽  
Low Mass ◽  
Low Mass Ratio

scholarly journals The low mass ratio contact binary system V728 Herculis

New Astronomy ◽  
2016 ◽  
Vol 46 ◽  
pp. 73-77 ◽  
Author(s):  
N. Erkan ◽  
B. Ulaş
Keyword(s):  
Binary System ◽  
Mass Ratio ◽  
Contact Binary ◽  
Low Mass ◽  
Low Mass Ratio

scholarly journals MULTICOLOR STUDY OF V1009 PER, A CLOSE BINARY SYSTEM AT THE BEGINNING OF THE OVERCONTACT PHASE, AND OF CRTS J031642.2+332639, A NEW BINARY SYSTEM IN THE SAME FIELD

2019 ◽  
Vol 55 (1) ◽  
pp. 65-72
Author(s):  
Raúl Michel ◽  
Francesco Acerbi ◽  
Carlo Barani ◽  
Massimiliano Martignoni
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Binary Systems ◽  
General Pattern ◽  
Close Binary System ◽  
Eclipsing Binaries ◽  
Close Binary ◽  
Mass Ratio ◽  
Period Variations ◽  
Contact Binaries

The first multicolor observations and light curve solutions of the eclipsing binary systems V1009 Per and CRTS J031642.2+332639 are presented. Using the 2005 version of the Wilson-Devinney code, both systems are found to be W UMa contact binaries. V1009 Per has a mass ratio of q = 0.362±0.002 and a shallow fill out parameter of f = 11.8 ± 0.6% while CRTS J031642.2+332639 has a mass ratio of q = 2.507±0.006 and a fill out of f = 13.6±0.4%. High orbital inclinations, i = 85◦.9 for V1009 Per and i = 83◦.2 for CRTS J031642.2+332639, imply that both systems are total eclipsing binaries and that the photometric parameters here obtained are reliable. Based on 16 times of minimum the orbital period variations of V1009 Per are discussed. The absolute dimensions of the systems are estimated and, from the log M − log L diagram, it is found that both components of the systems follow the general pattern of the W subtype W Ursae Majoris systems.

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.

scholarly journals Discovery of an M-type companion to the Herbig Ae Star V1787 Ori

2020 ◽  
Vol 501 (1) ◽  
pp. 1243-1252
Author(s):  
R Arun ◽  
Blesson Mathew ◽  
Sridharan Rengaswamy ◽  
P Manoj ◽  
Mayank Narang ◽  
...  
Keyword(s):  
Binary System ◽  
Adaptive Optics ◽  
Spectral Type ◽  
Template Matching ◽  
Binary Systems ◽  
Mass Ratio ◽  
Wide Binary ◽  
Star Forming ◽  
Low Mass ◽  
Low Mass Ratio

ABSTRACT The intermediate-mass Herbig Ae star V1787 Ori is a member of the L1641 star-forming region in the Orion A molecular cloud. We report the detection of an M-type companion to V1787 Ori at a projected separation of 6.66 arcsec (corresponding to 2577 au), from the analysis of VLT/NACO adaptive optics Ks-band image. Using astrometric data from Gaia DR2, we show that V1787 Ori A and B share similar distance (d ∼ 387 pc) and proper motion, indicating that they are physically associated. We estimate the spectral type of V1787 Ori B to be M5 ± 2 from colour–spectral type calibration tables and template matching using SpeX spectral library. By fitting PARSEC models in the Pan-STARRS colour–magnitude diagram, we find that V1787 Ori B has an age of 8.1$^{+1.7}_{-1.5}$ Myr and a mass of 0.39$^{+0.02}_{-0.05}$ M⊙. We show that V1787 Ori is a pre-main-sequence wide binary system with a mass ratio of 0.23. Such a low-mass ratio system is rarely identified in Herbig Ae/Be binary systems. We conclude this work with a discussion on possible mechanisms for the formation of V1787 Ori wide binary system.

Gravitational Radiation and the Evolution of Low Mass Binaries

1976 ◽  
Vol 73 ◽  
pp. 193-204 ◽  
Author(s):  
John Faulkner
Keyword(s):  
Mass Transfer ◽  
Angular Momentum ◽  
Binary System ◽  
Observational Study ◽  
Gravitational Radiation ◽  
Region Of Interest ◽  
Close Binary System ◽  
Close Binary ◽  
Theoretical Studies ◽  
Low Mass

Gravitational radiation of energy and angular momentum can modify and in some cases, control the evolution of a close binary system. The region of interest is briefly delineated. Recent work of the author and colleagues of relevance to this area is discussed, including theoretical studies of accretion, mass loss and mass transfer, and an observational study of a system, HZ 29 where gravitational radiation may dictate its behaviour.

scholarly journals Orbital properties of an unusually low-mass sdB star in a close binary system with a white dwarf

2012 ◽  
Vol 424 (3) ◽  
pp. 1752-1761 ◽  
Author(s):  
R. Silvotti ◽  
R. H. Østensen ◽  
S. Bloemen ◽  
J. H. Telting ◽  
U. Heber ◽  
...  
Keyword(s):  
Binary System ◽  
White Dwarf ◽  
Close Binary System ◽  
Close Binary ◽  
Low Mass

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.

Sign in / Sign up

Export Citation Format

Share Document