Light curve solutions of six eclipsing binaries at the lower limit of periods for W UMa stars

Kjurkchieva, D.; Dimitrov, D.; Ibryamov, S.

doi:10.1088/1674-4527/15/9/006

Cited by 7 publications

(7 citation statements)

References 27 publications

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“…This paper is continuation of our study of ultrashort-period binaries (Dimitrov & Kjurkchieva 2010, 2015; Kjurkchieva, Dimitrov, & Ibryamov 2015; Kjurkchieva & Dimitrov 2015; Kjurkchieva et al 2016). It presents results of our photometric and low-resolution spectral observations of 10 binaries with orbital periods within 5.1–5.5 h: NSVS 2175434; NSVS 2607629; NSVS 5038135; NSVS 8040227; NSVS 9747584; NSVS 4876238; ASAS 071829-0336.7 (further ASAS 0718-03); SWASP 074658.62+224448.5 (further SWASP 0746+22); NSVS 2729229; NSVS 10632802.…”

Section: Introductionsupporting

confidence: 56%

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Observations and Light Curve Solutions of Ultrashort-Period Eclipsing Binaries

Kjurkchieva

Dimitrov

Ibryamov

et al. 2018

Publ. Astron. Soc. Aust.

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Photometric observations in V and I bands and low-dispersion spectra of ten ultrashort-period binaries (NSVS 2175434, NSVS 2607629, NSVS 5038135, NSVS 8040227, NSVS 9747584, NSVS 4876238, ASAS 071829-0336.7, SWASP 074658.62+224448.5, NSVS 2729229, NSVS 10632802) are presented. One of them, NSVS 2729229, is newly discovered target. The results from modeling and analysis of our observations revealed that: (i) Eight targets have overcontact configurations with considerable fillout factor (up to 0.5) while NSVS 4876238 and ASAS 0718-03 have almost contact configurations; (ii) NSVS 4876238 is rare ultrashortperiod binary of detached type; (iii) all stellar components are late dwarfs; (iv) the temperature difference of the components of each target does not exceed 400 K; (v) NSVS 2175434 and SWASP 074658.62+224448.5 exhibit total eclipses and their parameters could be assumed as well-determined; (v) NSVS 2729229 shows emission in the Hα line. Masses, radii and luminosities of the stellar components were estimated by the empirical relation "period, orbital axis" for short-and ultrashort-period binaries. We found linear relations mass-luminosity and mass-radius for the stellar components of our targets.

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Section: Introductionsupporting

confidence: 56%

“…This paper is continuation of our study of ultrashort-period binaries (Dimitrov & Kjurkchieva 2010Kjurkchieva, Dimitrov, & Ibryamov 2015;; * Based on observations at NAO Rozhen. Kjurkchieva et al 2016).…”

Section: Introductionmentioning

confidence: 86%

Observations and Light Curve Solutions of Ultrashort-Period Eclipsing Binaries

Kjurkchieva

Dimitrov

Ibryamov

et al. 2018

Publ. Astron. Soc. Aust.

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“…Both diagrams (F) The light curve for the N112 system has already been studied. Kjurkchieva et al (2015) have obtained the following results using photometric observations in V and I c filters from the light curves for this system: q = 0.986(6), i = 74.36(26), T 1 = 4600(90), T 2 = 3969(70), f = 0.209. This study did not estimate the absolute parameters of the system.…”

Section: Discussionmentioning

confidence: 89%

“…Besides, N581 was classified as a W UMa-type in the Northern Sky Variability Survey (NSVS) variables automated classification catalog (Hoffman et al 2009). Furthermore, in the Qian (2020), andKjurkchieva et al (2015) studies, N112 was classified as an Eclipsing Binary (EB), and its V band magnitude is given as 13.66 mag .…”

Section: Introductionmentioning

confidence: 99%

Global Parameters of Eight W UMa-type Binary Systems

Poro,

Tanriver,

Michel

et al. 2024

PASP

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Multiband photometric investigations for eight binary systems of the W Ursae Majoris-type are presented. Six systems are presented for the first time to analyze their light curves. All the analyzed systems have a temperature below 5000 K and an orbital period of less than 0.28 days. We extracted primary and secondary minima from the ground-based observations of these systems. According to a few observations reported in the literature, linear fits were considered in the O − C diagrams, and new ephemerides were presented. Light curve solutions were performed using the PHysics Of Eclipsing BinariEs code. The results of the mass ratio and fillout factor indicate that the systems are contact binary stars. Six of them showed the O’Connell effect, and a cold starspot on each companion was required for light curve solutions. Their absolute parameters were estimated and evaluated by two other methods. In this study, the empirical relationship between the orbital period and semimajor axis was updated using a sample consisting of 414 contact binary systems and the Monte Carlo Markov Chain approach. Also, using Machine Learning and the Artificial Neural Network model, the relationship between P–T 1–M 1 was updated for a better estimation of the mass of the primary star.

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“…Recently, a new statistical study reveals that the real short-period limit for W UMa-type stars is about 0.2 days (Qian et al 2017). The investigation of binary stars below this limit (0.2 days) can provide very valuable information on the formation and evolution of contact binaries; for example, the angular momentum and mass loss, and the final merging of EBs (Qian et al 2015a;Kjurkchieva et al 2015). To date, only a few main-sequence EBs with orbital periods shorter than 0.2 days were detected and well investigated, such as SDSS J001641-000925 (P=0.1985615 days, Davenport et al 2013;Qian et al 2015b), BW3 V38 (P=0.1984 days, Maceroni & Montalbán 2004), and GSC 2314-0530 (P=0.192636 days, Dimitrov & Kjurkchieva 2010.…”

Section: Introductionmentioning

confidence: 99%

A Detached Eclipsing Binary with a Period Shorter than 0.2 Days in a Triple System

Zhang

Qian

Zhi

et al. 2019

PASP

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W UMa-type binary stars have an apparent short-period cutoff around 0.2 days. Close binaries with orbital periods shorter than this limit are very useful for understanding the formation and evolution of this type of binaries. 2MASS J11553339+3544399 (hereafter J1155) is a red-dwarf binary with a period of 0.199724 days. Multicolor (V, R, R c , I, I c , W) light curves (LCs) for the ultrashort-period eclipsing binary (EB) J1155 are presented and analyzed by using the Wilson-Devinney (W-D) code. We find that J1155 belongs to a rare group of detached red-dwarf EB with periods below the period limit of contact binaries (the other two are BW03 V38 and GSC 2314-0530). It has a high-mass ratio of 0.90. The primary component (the more massive and hotter star) is filling 90% of the critical Roche lobe, while the secondary one is filling about 84.8%. The masses and radii of the two components are estimated as M 1 =0.475±0.035 M e , M 2 =0.441±0.044 M e , R 1 =0.516±0.089 R e , and R 2 =0.491±0.105 R e , respectively. By analyzing all available times of light minimum, the orbital period changes of the binary system are investigated for the first time. We find that the (O − C) (observed-calculated) diagram shows a cyclic oscillation with an amplitude of 0.00326 days and a period about 9.84 years. This oscillation is explained as the light-travel time effect (LTTE) via the presence of a third body. The mass of the third component in the triple system is computed to be M 3 sin(i′)∼0.127 M e . The orbital distance between the central binary and the tertiary component is about 4.0 au. It is possible that the third body and the magnetic braking may play important roles in the formation and evolution of J1155 by drawing angular momentum from the central system.

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Light curve solutions of six eclipsing binaries at the lower limit of periods for W UMa stars

Cited by 7 publications

References 27 publications

Observations and Light Curve Solutions of Ultrashort-Period Eclipsing Binaries

Observations and Light Curve Solutions of Ultrashort-Period Eclipsing Binaries

Global Parameters of Eight W UMa-type Binary Systems

A Detached Eclipsing Binary with a Period Shorter than 0.2 Days in a Triple System

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