RW Doradus: a photometric study

Marton, S.; Grieco, A.; Sisteró, R. F.

doi:10.1093/mnras/240.4.931

Cited by 8 publications

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“…However, they found V 0 = 25 km s −1 , which is somewhat smaller than the V 0 = 66.5 km s −1 given by Hilditch, Hill, and Bell (1992). Marino et al (2007) reported that some light curves of RW Dor exhibited asymmetry, being similar to the results published by Marton, Grieco, and Sistero (1989). They also recomputed the spectroscopic mass ratio by using the radial velocities given by Hilditch, Hill, and Bell (1992) and Duerbeck and Rucinski (2007).…”

Section: Introductionmentioning

confidence: 60%

“…Additionally, it was found that the light curves of RW Dor exhibited a significant difference in the depths of the minima and showed variation. Marton, Grieco, and Sistero (1989) explained the asymmetry in the light curves as a hot spot on the cooler and more massive component located near the neck connecting the stars, while Kaluzny and Caillault (1989) reported that their light curves were only marginally asymmetric and did not show any scatter beyond the observational errors.…”

Section: Introductionmentioning

confidence: 99%

“…The first photographic times of light minima were reported by Hertzsprung (1928), who gave an orbital period of 0.143 d. Later, eclipse times were obtained by many authors (e.g., Russo et al 1984;Marton et al 1989;Kaluzny & Caillault 1989;Ogloza & Zakrzewski 2004;Marino et al 2007) and the linear ephemeris of the binary was also corrected. The complete light curves were analyzed with the Wilson-Devinney method (Wilson & Devinney 1971) by Marton, Grieco, and Sistero (1989) and Kaluzny and Caillault (1989), who determined the photometric elements independently. Those solutions indicated that RW Dor belongs to a W-subtype contact binary with components not in poor thermal contact, as predicted by the thermal relaxation oscillation theory (Lucy & Wilson 1979).…”

Section: Introductionmentioning

confidence: 99%

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RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Sarotsakulchai

Qian

Soonthornthum

et al. 2019

Publications of the Astronomical Society of Japan

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New CCD photometric light curves of the short-period (P = 0.285 d) eclipsing binary RW Dor are presented. The observations were performed with the PROMPT-8 robotic telescope at CTIO in Chile between 2015 March and 2017 March. Other eclipse timings were obtained from the 2.15 m JS telescope at CASLEO, San Juan, Argentina in 2011 December. Based on a light curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f ∼ 11% and a high mass ratio q ∼ 1.587 (1/q = 0.63), where the hotter component is the less massive one (M 1 ∼ 0.52 M and M 2 ∼ 0.82 M ). For orbital-period investigation, 15 new eclipse times and those previously published were compiled. O − C analysis with very weak evidence suggests that a long-term decrease in period with a rate of dP/dt = −9.61 × 10 −9 d yr −1 is superimposed on a cyclic variation (A 3 = 0.0054 d and P 3 = 49.9 yr). The long-term decrease can be interpreted as mass transfer from the more massive component to the less massive one, or combined with angular momentum loss via magnetic braking. In addition, the marginal contact phase, high mass ratio (1/q > 0.4), and long-term decrease in period all suggest that RW Dor is a newly formed contact binary via Case A mass transfer, and it will evolve into a deeper normal contact binary. If the cyclic change is correct, the light travel-time effect via the presence of a cool third body will be a more plausible explanation for this.

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Section: Introductionmentioning

confidence: 60%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Sarotsakulchai

Qian

Soonthornthum

et al. 2019

Publications of the Astronomical Society of Japan

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“…On the other hand, our phase coverage is very sparse, with only three observations not falling within the conjunctions. Hilditch et al (1992) assumed a spectral type of K1 V following Marton et al (1989). The Tycho-2 color, B À V ¼ 0:66, suggests an earlier spectral type of about G4/5 V with V max ¼ 10:97.…”

Section: Rw Dormentioning

confidence: 99%

Radial Velocity Studies of Southern Close Binary Stars. II. Spring/Summer Systems

Duerbeck

Ruciński

2006

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Radial velocity measurements and sine-curve fits to the orbital velocity variations are presented for 14 close binary stars, S Ant, TT Cet, TW Cet, AA Cet, RW Dor, UX Eri, YY Eri, BV Eri, CT Eri, SZ Hor, AD Phe, TY Pup, HI Pup, and TZ Pyx. All are double-lined binaries, and all except the last one are contact binaries. The orbital data must be considered preliminary because of the relatively small number of observations (6Y12), a circumstance that is partly compensated by the good definition of the broadening functions used for the radial velocity determinations.

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“…Full photometric coverage of the variable was reported by Kaluzny & Caillault (1989) and Marton, Grieco & Sistero (1989), together with summaries of previous work. These mention variability of the light curve shape as well as the significant difference in eclipse depths.…”

Section: Introductionmentioning

confidence: 99%

Observation and Analysis of RW Doradus

Marino¹,

Walker

Bembrick³

et al. 2007

Publ. – Astron. Soc. Aust

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Photometry of the short-period (P ∼0.285 d) low-mass (M 1 ∼0.67, M 2 ∼0.48 M ) W UMa-type eclipsing binary RW Dor, mainly involving a good series of observations in 1987-88, using standard B and V filters at the Auckland Observatory, is examined. Analysis via light curve fittings alone permits both transit (near main sequence) and occultation (W-type contact binary) solutions. Consideration of proximity or other effects on the relatively small number of measured radial velocities gives rise to a more detailed review of the alternatives, though the (W-type) configuration determined by Hilditch, Hill & Bell (1992) is still confirmed. Further implications of this configuration are examined, given an apparent general trend to period decrease ( P/P ∼6 × 10 −11 ), and some light curve asymmetry. This is consistent with the initially low-mass companion, Case-B scenario of Budding (1984). The evidence does suggest irregularity of the period variation however, and further detailed surveillance, including more spectroscopy, is desirable.

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RW Doradus: a photometric study

Cited by 8 publications

References 0 publications

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Radial Velocity Studies of Southern Close Binary Stars. II. Spring/Summer Systems

Observation and Analysis of RW Doradus

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