On the origin of W UMa type contact binaries – a new method for computation of initial masses

Yıldız, Mutlu; DOĞAN, Taylan

doi:10.1093/mnras/stt028

Cited by 108 publications

(92 citation statements)

References 61 publications

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“…The primary star lies in the mainsequence band, while the secondary (less massive) is oversized and oveluminous for its mass. Actually, the radius of the secondary is 1.08 ± 0.02  R , nearly twice that of a mainsequence star with M = 0.43 ± 0.02  M , and follows the general radius difference of other A-type W UMa binaries found by Yildiz & Doğan (2013). In combination with the temperature difference between the components, there has probably been a past epoch of mass transfer.…”

supporting

confidence: 68%

“…By applying their method to HI Dra, we found that the initial mass of the currently less massive component (0.43 ± 0.02  M ) would be 2.25 ± 0.07  M , that is, HI Dra should have evolved to an A subtype as predicted by our best model. With an initial mass of the HI Dra currently massive component calculated as 1.11 ± 0.03  M , the calculated initial total mass of the system (3.36  M ) is in good agreement with the mean total initial mass for a typical A subtype of 3  M (Yildiz & Doğan 2013). Moreover, following the procedure described by Yıldız (2014), we estimated the current age (the summation of the durations of three phases: detached, semidetached, and contact) of the HI Dra binary system to be approximately 2.4 Gyr.…”

supporting

confidence: 61%

“…Recently, Yildiz & Doğan (2013) developed a method for the computation of initial masses of contact binaries based on stellar modeling with mass loss from luminosity excess. Their main assumption is that the mass transfer starts near or after the TAMS phase of the initially massive component, which is the progenitor of the currently less massive component.…”

mentioning

confidence: 99%

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Absolute Parameters and Physical Nature of the Low-Amplitude Contact Binary Hi Draconis

Παπαγεωργίου

Christopoulou

2015

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We present a detailed investigation of the low-amplitude contact binary HI Dra based on the new VR c I c CCD photometric light curves (LCs) combined with published radial velocity (RV) curves. Our completely covered LCs were analyzed using PHOEBE and revealed that HI Dra is an overcontact binary with low fill-out factor f = 24 ± 4 (%) and temperature difference between the components of 330 K. Two spotted models are proposed to explain the LC asymmetry, between which the A subtype of W UMa type eclipsing systems, with a cool spot on the less massive and cooler component, proves to be more plausible on evolutionary grounds. The results and stability of the solutions were explored by heuristic scan and parameter perturbation to provide a consistent and reliable set of parameters and their errors. Our photometric modeling and RV curve solution give the following absolute parameters of the hot and cool components, respectively:Based on these results the initial masses of the progenitors (1.11 ± 0.03  M and 2.25 ± 0.07  M , respectively) and a rough estimate of the age of the system of 2.4 Gyr are discussed.

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supporting

confidence: 68%

supporting

confidence: 61%

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Absolute Parameters and Physical Nature of the Low-Amplitude Contact Binary Hi Draconis

Παπαγεωργίου

Christopoulou

2015

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“…It is observed that A-subtype contact binaries are dominant for q < 0.25, while W-subtype contact binaries exist in the early stage of evolution with q > 0.4 and both the subtypes are equally common in the region 0.25 < q < 0.4 (Yildiz & Dogan, 2013). The energy transfer in the common convective envelope of the contact binaries may occur in the deeper layers for A-subtype but in the outermost layers for W-subtype.…”

Section: Discussionmentioning

confidence: 96%

Long-term photometric study of a faint W UMa binary in the direction of M31

Joshi

Rukmini

2017

Res. Astron. Astrophys.

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We carry out a re-analysis of the photometric data in R c I c bands which was taken under the Nainital Microlensing Survey during 1998 to 2002 with the aim to detect gravitational microlensing events in the direction of M31. Here, we do photometric analysis of a faint W UMa binary CSS J004259.3 + 410629 identified in the target field. The orbital period of this star is found to be 0.266402±0.000018 day. The photometric mass ratio, q, is found to be 0.28 ± 0.01. The photometric light curves are investigated using the Wilson-Devinney (WD) code and absolute parameters are determined using empirical relations which provide masses and radii of the binary as M 1 = 1.19 ± 0.09M ⊙ , M 2 = 0.33 ± 0.02M ⊙ and R 1 = 1.02 ± 0.04R ⊙ , R 2 = 0.58 ± 0.08R ⊙ based on the R c band data. Almost similar values are found by analysing I c band data. From the photometric light curve examination, the star is understood to be a low mass-ratio overcontact binary of A-subtype with a high fill-out factor of about 47%. The binary system is found to be located approximately at a distance of 2.64 ± 0.03 kpc having a separation of 2.01 ± 0.05 R ⊙ between the two components.

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“…On the other hand, when the more massive star obscures the less massive one at the primary eclipse, it is called W-subtype (Binnendijk 1970(Binnendijk , 1977. At present, there are two conflicting arguments that W-subtypes evolve into A-subtypes (Flannery 1976;Lucy 1976;Wilson 1978;Mochnacki 1981;Hilditch 1989;Awadalla & Hanna 2005;Eker et al 2006;Gazeas & Niarchos 2006) and that there is no evolutionary link between them (Maceroni & Van't Veer 1996;Yildiz & Doğan 2013).…”

Section: Introductionmentioning

confidence: 99%

The First Photometric Study of NSVS 1461538: A New W-subtype Contact Binary with a Low Mass Ratio and Moderate Fill-out Factor

Kim¹,

Kim²,

Song³

et al. 2016

Journal of Astronomy and Space Sciences

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On the origin of W UMa type contact binaries – a new method for computation of initial masses

Cited by 108 publications

References 61 publications

Absolute Parameters and Physical Nature of the Low-Amplitude Contact Binary Hi Draconis

Absolute Parameters and Physical Nature of the Low-Amplitude Contact Binary Hi Draconis

Long-term photometric study of a faint W UMa binary in the direction of M31

The First Photometric Study of NSVS 1461538: A New W-subtype Contact Binary with a Low Mass Ratio and Moderate Fill-out Factor

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