A Charge-Coupled Device Photometric Study of South Hemispheric Contact Binary Ae Phoenicis

He, J.-J.; Qian, S.‐B.; Lajús, E. Fernández; Fariña, C.

doi:10.1088/0004-6256/138/5/1465

Cited by 9 publications

(7 citation statements)

References 10 publications

(23 reference statements)

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“…This means that the AE Phe system shows a long-term continuous period increase. The period increase rate that we attained is 4.5 times slower than what was reported in [2], which yielded a rate of dP/dt = 6.17(±0.44) × 10 −8 days/year. The O-C diagram comparison between this paper and [2] is shown in figure 3.…”

Section: O-c Diagramcontrasting

confidence: 62%

“…al. (2009) [2]; and this paper. To analyze the O-C diagram, we gave a weighting scheme based on the data acquisition instruments.…”

Section: O-c Diagrammentioning

confidence: 69%

“…The AE Phe system has been identified as a W-UMa type binary with a short period of 0.362 days. The most recent analysis of the AE Phe system was reported by He et. al (2009) [2].…”

Section: Introductionmentioning

confidence: 99%

“…The most recent analysis of the AE Phe system was reported by He et. al (2009) [2]. They presented the photometric solutions and the O-C diagram analysis of AE Phe.…”

Section: Introductionmentioning

confidence: 99%

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Conservative mass transfer on eclipsing binary AE Phe from O-C diagram analysis

Vidante

Malasan

2022

J. Phys.: Conf. Ser.

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Eclipsing binary is an edge-on binary system where the components appear to be eclipsing one another. Eclipsing binaries therefore give a lot of information on the systems’ behavior, one of them from their period change. O-C diagram exhibits the deviation of the observed time of minimum from the calculated ones and its analysis will reveal the responsible mechanism, such as a hidden third component, apsidal motion, and mass transfer. AE Phe (V = 8.15 mag and spectral class G0V) is a W UMa W-type binary. Previous studies of its degree of contact have revealed AE Phe to be a shallow-contact binary. Photometric data were taken using PROMPT (Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes), CTIO on October 4th, 2013 on four filters: B, V, R, and I. The Kwee and van Woerden (1956) method was also used to determine AE Phe’s time of minimum. Analysis of the O-C diagram (taken from 1975 toward our observation) suggest that the period of AE Phe shows a long-term continuous increase. These period increase and degree of contact suggest that AE Phe is undergoing thermal relaxation oscillation (TRO) and is evolving to a broken-contact phase, with a possibility of angular momentum loss (AML) through magnetic braking.

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Section: O-c Diagramcontrasting

confidence: 62%

“…al. (2009) [2]; and this paper. To analyze the O-C diagram, we gave a weighting scheme based on the data acquisition instruments.…”

Section: O-c Diagrammentioning

confidence: 69%

“…The AE Phe system has been identified as a W-UMa type binary with a short period of 0.362 days. The most recent analysis of the AE Phe system was reported by He et. al (2009) [2].…”

Section: Introductionmentioning

confidence: 99%

“…The most recent analysis of the AE Phe system was reported by He et. al (2009) [2]. They presented the photometric solutions and the O-C diagram analysis of AE Phe.…”

Section: Introductionmentioning

confidence: 99%

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Conservative mass transfer on eclipsing binary AE Phe from O-C diagram analysis

Vidante

Malasan

2022

J. Phys.: Conf. Ser.

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“…The fill-out factor is about 12.86%(±0.73%) indicating that HH Boo is a shallow-contact binary system. The observational properties of HH Boo are similar to some EW-type contact binaries such as AE Phe [45], V524 Mon [46], NSVS 2669503 [47], DE Lyn [48], AQ Boo [49], GK Aqr [50], and V532 Mon [51]. All of them are W-type shallow-contact systems with < 20% that are at the beginning phase of contact (e.g., [37]).…”

Section: Discussionmentioning

confidence: 75%

New Photometric Investigation of the Solar-Type Shallow-Contact Binary HH Bootis

Qian

Soonthornthum

et al. 2019

Advances in Astronomy

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The short-period solar-type contact binary HH Boo was monitored photometrically for about 8 years. It is found that the CCD light curves in the B, V, R, and I bands obtained in 2010 are symmetric, while the multicolor light curves observed in 2011 and 2012 by several investigators showed a positive O’Connell effect where the maxima following the primary minima are higher than the other ones. This indicates that the light curve of the solar-type contact binary is variable. By analyzing our multicolor light curves with the Wilson-Devinney code (W-D code), it is confirmed that HH Boo is a W-type shallow-contact binary system with a mass ratio of q = 1.703(31) and a degree of contact factor of f = 12.86%(0.73%). By including 109 new determined times of light minimum together with those compiled from the literature, it is detected that the O-C diagram shows a cyclic oscillation with a period of T3 = 6.58(11) yr and an amplitude of A3 = 0.0018(1) d. The cyclic change may reveal the presence of an extremely cool third body orbiting the central binary.

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