Photometric study of AE Phoenicis

Williamon, R. M.

doi:10.1086/111726

Cited by 6 publications

(6 citation statements)

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“…Secondary minimum = HJD2440857.8162 + 0. d 36237459 × E. Williamon (1975) and Grønbech (1976) found that the light curves of AE Phe were asymmetric from their observations. Grønbech (1976) found that a maximum brightness occurs at phase 0.25, which is 0.02 mag brighter in the I band.…”

Section: Introductionmentioning

confidence: 93%

“…To study the variations of the orbital period, we collect all the available photoelectric and CCD times of light minimum from the literature (Williamon 1975;Grønbech 1976;Walter & Duerbeck 1988 (hereafter W88); M94). We revised the M94 published JD times of light minimum to HJD.…”

Section: Orbital Period Change Of Ae Phementioning

confidence: 99%

“…Grønbech (1976) found that a maximum brightness occurs at phase 0.25, which is 0.02 mag brighter in the I band. Williamon (1975) found that the secondary eclipse was asymmetric. In Figure 1, one can see that the asymmetries of the B, V, R, and I bands are all less than 0.01 mag.…”

Section: Photometric Solutions Of Ae Phementioning

confidence: 99%

“…The photometric investigations of Duerbeck (1978) indicate that the orbit of AE Phe is elliptical. The first photoelectric observations in the UBV system were published by Williamon (1975) who determined system elements by the Russell-Merrill method (Russell & Merrill 1952). By combining 35 photographically determined times of minimum reported by Avery & Sievers (1968), Williamon determined a period of 0. d 36237459(±0.00000025) for AE Phe and did not find any period change over a short period of time.…”

Section: Introductionmentioning

confidence: 99%

“…Grønbech (1976) found that a maximum brightness occurs at phase 0.25, which is 0.02 mag brighter in the I band. Williamon (1975) found that the secondary eclipse was asymmetric. One year later, Grønbech (1976) used all available times of primary minimum and improved the linear ephemeris as…”

Section: Introductionmentioning

confidence: 99%

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

He¹,

Qian²,

Lajús³

et al. 2009

The Astronomical Journal

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The complete charge-coupled device light curves in B, V, R, and I bands of the short-period binary system, AE Phe, are presented. It is found that the light curves of AE Phe belong to typical EW-type light variation. Photometric solutions were derived by using the 2003 version of the Wilson-Devinney code. It showed that AE Phe is a Wsubtype shallow-contact system (f = 14.6%(±0.5%)) with a mass ratio of q = 2.5491(±0.0092). The temperature difference between the two components is 227 K. Analysis of the O − C curve suggests that the period of AE Phe shows a long-term continuous increase at a rate of dP /dt = +6.17(±0.44) × 10 −8 days year −1 . The longterm period increase, the marginal-contact configuration, and the astrophysical parameters of the binary system, all suggest that it is a shallow-contact binary undergoing a thermal relaxation oscillation evolving into a detached binary.

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Section: Introductionmentioning

confidence: 93%

Section: Orbital Period Change Of Ae Phementioning

confidence: 99%

Section: Photometric Solutions Of Ae Phementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

“…Grønbech (1976) found that a maximum brightness occurs at phase 0.25, which is 0.02 mag brighter in the I band. Williamon (1975) found that the secondary eclipse was asymmetric. One year later, Grønbech (1976) used all available times of primary minimum and improved the linear ephemeris as…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

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

He¹,

Qian²,

Lajús³

et al. 2009

The Astronomical Journal

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Surface images of the short period contact binary AE Phe

Barnes¹,

Lister²,

Hilditch³

et al. 2004

Astron Nachr

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We present high resolution Doppler images of the short period (P = 0.362 d) contact binary AE Phe. Using least squares deconvolution, we make use of the information content of the several thousand lines in each echelle spectrum to obtain the necessary S/N and time resolution required to resolve individual starspot features. A single pair of rotationally broadened profiles (free of sidelobes due to blending) with a typical S/N of 3000 - 4000 per spectrum is thus obtained. With 300 sec exposures we achieve a cadence of 350 sec which is equivalent to sampling the rotation phase every 4degrees. We derive images for four nights of data which reveal starspots at most latitudes on both components of the common envelope system. Individual starspots evolve significantly on very short timescales, of order one day; significantly faster than the week timescales found on active single stars and the Sun

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An Analysis of the Light Changes of W UMa-Type Systems in the Frequency Domain

Niarchos

1981

Photometric and Spectroscopic Binary Systems

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Photometric study of AE Phoenicis

Cited by 6 publications

References 0 publications

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

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

Surface images of the short period contact binary AE Phe

An Analysis of the Light Changes of W UMa-Type Systems in the Frequency Domain

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