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Rovithis‐Livaniou, H.; Fragoulopoulou, E.; Sergis, N.; Rovithis, P.; Kranidiotis, A.

doi:10.1023/a:1002734605735

Cited by 34 publications

(39 citation statements)

References 11 publications

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“…Moreover, the P(E) function does not depend on the ephemeris formula used, as has been proven by Kalimeris et al (1994b); so, periodic terms, if any, can be found by applying Fourier transforms to the P(E) function. The results achieved so far show that in most of the examined cases the computed periodic terms correspond to the time interval covered by the observations and to half of it (Rovithis-Livaniou et al, 2001). These results rise a lot of questions with regard to the possible existence of third bodies associated with close binaries, except of course those cases, where third bodies are confirmed by other means (e.g., Hendry and Mochnacki 1998).…”

Section: Discussionmentioning

confidence: 65%

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Period Changes of Close Binary Systems

Rovithis‐Livaniou¹

2005

Astrophys Space Sci

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Section: Discussionmentioning

confidence: 65%

“…A review concerning all analysis methods of (O − C) diagrams of any close eclipsing binary and a comparison between traditional and new techniques has been presented by Rovithis-Livaniou (2001).…”

Section: Orbital Period Analysis Techniquesmentioning

confidence: 99%

Period Changes of Close Binary Systems

Rovithis‐Livaniou¹

2005

Astrophys Space Sci

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“…To compute the amplitude of the period oscillation of V346 Cyg shown in Figure 1, one could use the following equation (Rovithis-Livaniou et al 2000),…”

Section: Magnetic Activitymentioning

confidence: 99%

Period Variation Study of the Neglected Algol Eclipsing Binary System V346 Cygnius

Hanna¹

2014

Journal of The Korean Astronomical Society

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Abstract:We present the first period variation study for the Algol eclipsing binary V346 Cyg by constructing the (O − C) residual diagram using all the available precise minima times. We conclude that the period variation can be explained by a sine-like variation due to the presence of a third body orbiting the binary in about 68.89 ± 4.69 years, together with a long-term orbital period decrease (dP/dt = −1.23 × 10 −7 day/yr) that can be interpreted to be due to slow mass loss from the δ-Scuti primary component. The sinusoidal variation may also be explained by using the the Applegate (1992) mechanism involving cyclic magnetic activity due to star-spots on the secondary component. The present preliminary solution needs more precise photometric observations to be confirmed.

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“…Spectroscopic observations were made by Sanford (1934). The period studies of AK Her were performed by Schmidt & Herczeg (1959), Binnendijk (1961), Herczeg (1962), Purgathofer & Prochazka (1966), Woodward & Wilson (1977), Barker & Herczeg (1979), Bookmyer & Kaitchuck (1979), Rafert (1982), Glownia (1985), Tunca et al (1987), and Rovithis-Livaniou et al (1999). So far most of the studies investigated variations Send offprint requests to: L. Li, e-mail: llf@cosmos.ynao.ac.cn Table 3 is only available in electronic form at http://www.edpsciences.org in the period, and the detected periodicities range from 58 to 78 years.…”

Section: Introductionmentioning

confidence: 99%

“…Thus, the results have little physical meaning. We have collected all available minimum times which span an interval of 76.36 years, and correct five minimum times which Rovithis-Livaniou et al (1999) have adopted. Based on these minima, we again investigated the period variation, obtaining a result different from previous studying.…”

Section: Introductionmentioning

confidence: 99%

Research NoteThe W Ursae Majoris system AK Herculis

Zhang

Han

2001

A&A

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Abstract.A detailed study of the period and the light-curve of the eclipsing binary AK Her is presented. Based on the study of the (O-C) curve, we find that the period variation of the system contains a component of a long-term decrease, and three other components of periodical variation. Our result is very different from that of other investigators. We compare light curves obtained by other groups and find that the light curve of the system has changed considerably. Based on the analysis, we investigate the physical mechanisms which may underlie the variations of the period and the light curve and obtain some new conclusions. According to the characteristics of rapid light variation of the system, we conclude that the rapid change is probably caused by pulsation of the common envelope, and that the physical mechanism causing the pulsation may be mass transfer between the two components. In addition, we find that the amplitude of the light curve variation is almost proportional to the rate of the period variation. Finally, the trends in the evolution of the system are discussed.

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Cited by 34 publications

References 11 publications

Period Changes of Close Binary Systems

Period Changes of Close Binary Systems

Period Variation Study of the Neglected Algol Eclipsing Binary System V346 Cygnius

Research NoteThe W Ursae Majoris system AK Herculis

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