U,B,V Light Curves of the Short-Period Solar-Type Eclipsing Binary, V417 Aquilae

Samec, R. G.; Pauley, B.; Carrigan, B.

doi:10.1086/118262

Cited by 12 publications

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“…Times of light minimum of V417 Aql were collected by Samec et al (1997), kindly provided by Dr. R. D. Samec. After their compilation, some photoelectric or CCD eclipse times were published (see Table 2).…”

Section: Variations Of the O-c Curvementioning

confidence: 99%

“…given by Samec et al (1997) was misprinted, it was used to calculate the O-C values of all the times of minimum light. The corresponding (O-C) diagram is shown in Fig.…”

Section: Variations Of the O-c Curvementioning

confidence: 99%

“…Kämper (1984) published 17 times of light minimum and presented the first period study of the binary system. The recent period studies by Samec et al (1997) and Pauley et al (1996) showed that two constant periods before HJD 2 433 000 and for modern era were connected by a continuous but smooth period decrease taking place over 24 years. Note, however, that the ephemeris in Eq.…”

Section: Introductionmentioning

confidence: 97%

“…A B − V color index of 0.62 obtained by Koch (1974) indicates that it is a solar type star. Normal complete photoelectric light curves in B and V were published by Faulkner (1983) who also gave a linear ephemeris: Min.I(HJD) = 2445554.7241 + 0.3703072 × E. Recently, high-precision photometric light curves (in U, B, and V) were published by Samec et al (1997). They gave solutions of geometric elements with the Wilson-Devinney (W-D) method.…”

Section: Introductionmentioning

confidence: 99%

“…Note, however, that the ephemeris in Eq. (2) of the paper by Samec et al (1997), based on the recent minima, is misprinted and should read Min.I(HJD) = 2 449 546.4979 + 0.3703119 × E, as in Pauley et al (1996). In order to understand the evolutionary state of V417 Aql and to look for cyclic variations in the orbital periods of overcontact binary systems, the properties of period changes of V417 Aql are investigated in detail.…”

Section: Introductionmentioning

confidence: 99%

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A period investigation of the overcontact binary system V417 Aquilae

Qian

2003

A&A

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Abstract.A detailed orbital period investigation of the short-period (P = 0.d 37) W UMa type star, V417 Aql, is presented based on the analysis of its O-C data. It is shown that the period change of the binary system is continuous. A periodic variation, with a period of 42.4 years and an amplitude of 0.d 0130, is found superimposed on a long-term period decrease (dP/dt = −5.50 × 10 −8 days/year). The period oscillation can be explained either by the light-time effect via the presence of an unseen third body or by magnetic activity cycles of the components. V417 Aql is a W-type overcontact binary system with a low mass ratio of q = 0.36. The long-term period variation is in agreement with the conclusion of Qian (2001b) that a low-mass ratio W-type system usually shows a secular period decrease. This suggests that V417 Aql is on the AML-controlled stage of the evolutionary scheme proposed by Qian (2001b). Meanwhile, the light-curve paradox encountered by TRO theory is discussed.

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Section: Variations Of the O-c Curvementioning

confidence: 99%

“…given by Samec et al (1997) was misprinted, it was used to calculate the O-C values of all the times of minimum light. The corresponding (O-C) diagram is shown in Fig.…”

Section: Variations Of the O-c Curvementioning

confidence: 99%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

A period investigation of the overcontact binary system V417 Aquilae

Qian

2003

A&A

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A critical review of period analyses and implications for mass exchange in W UMa eclipsing binaries: Paper 4

Nelson¹,

Terrell

Milone

2023

New Astronomy Reviews

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A possible relation between the period change and the mass ratio for W-type contact binaries

Qian

2001

Monthly Notices of the Royal Astronomical Society

122

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Orbital period changes of eight W‐type contact binaries (TY Boo, BH Cas, AD Cnc, TX Cnc, RZ Com, LS Del, BB Peg and AA UMa) are presented based on the analysis of their O–C curves. It is found that the periods of the five systems TY Boo, TX Cnc, RZ Com, LS Del and AA UMa show secular increase. For BB Peg, its period increase rate has been revised. For AD Cnc, weak evidence also shows that its orbital period is increasing. For the remaining BH Cas, the three times of light minimum given by Agerer & Hubscher indicate that, recently, its period has been increasing. However, the properties of the period need further study. The mass ratios of all the systems are larger than 0.4. The period increases of the systems may suggest that the W‐type W UMa stars with high mass ratio usually show their period increase. In order to check this conclusion, secular period changes of 30 W‐type contact binaries have been collected from the literature. It is found that systems showing period increase usually have a higher mass ratio , and the periods of low‐mass ratio systems are varying in a secular decrease. This strongly suggests that a relation between the orbital period variation and the mass ratio for W‐type contact binaries may exist. If the secular period change is caused by conservative mass transfer between the components, this relation may suggest that the evolution of the W‐type systems is oscillation around a critical mass ratio . However this is highly speculative. On the other hand, the relation may be potentially strong observational evidence for Rahunen's conclusion that angular momentum loss (AML) may enable the components of a contact binary to remain in good contact throughout the thermal relaxation oscillation (TRO) cycle. This connection could be explained by the combination of the TRO and the variable AML via the change of depth of contact, which needs further studies observationally and theoretically.

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U,B,V Light Curves of the Short-Period Solar-Type Eclipsing Binary, V417 Aquilae

Cited by 12 publications

References 0 publications

A period investigation of the overcontact binary system V417 Aquilae

A period investigation of the overcontact binary system V417 Aquilae

A critical review of period analyses and implications for mass exchange in W UMa eclipsing binaries: Paper 4

A possible relation between the period change and the mass ratio for W-type contact binaries

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