Recent photometry of CG Cygni

Naftilan, S. A.; Grillmair, Carl J.; Trager, G. B.

doi:10.1086/114301

Cited by 10 publications

(11 citation statements)

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“…They concluded that the orbital period of the system appears to have lengthened and to be continuously changing since the late 1960s. Naftilan et al (1987) confirmed this finding and suggested a period change of 4.15 × 10 −6 s/day. Hall (1991) updated the O-C curve and suggested that the mean brightness outside eclipse and the orbital period vary with the same cycle length of about 50 yr, on the basis of multiple linear fits.…”

Section: Eclipse Timings and Period Studysupporting

confidence: 72%

“…These workers have shown that the light curve of CG Cyg changes over short and long time intervals. Naftilan et al (1987) found that the mean light level outside eclipse increased between 1964 and 1976, after which the brightening of the mean light level halted. Sowell et al (1987) confirmed this result, noting that the mean light level outside eclipse increased by 15% rather uniformly between 1964 and 1977.…”

Section: Introductionmentioning

confidence: 98%

“…177 in the catalog of Chromospherically Active Binary Stars (Strassmeier et al 1993). Since its eclipsing nature was discovered by Williams (1922), many light curves have been obtained by various authors (Yü 1923;Milone et al 1979;Jassur 1980;Sowell et al 1987;Naftilan et al 1987;Bedford et al 1987;Dapergolas et al 1988Dapergolas et al , 1989aDapergolas et al ,b, 1994Zeilik et al 1989Zeilik et al , 1991Kjurkchieva et al 2003). These workers have shown that the light curve of CG Cyg changes over short and long time intervals.…”

Section: Introductionmentioning

confidence: 99%

“…Initial studies assumed that O-C values can be fit with a parabola (cf. Milone et al 1979;Naftilan et al 1987). Then, Hall (1991) represented the O-C values with four straight-line segments, i.e.…”

Section: Introductionmentioning

confidence: 99%

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Long-term luminosity variations and period changes in CG Cygni

Afşar¹,

Heckert²,

İbanoǧlu³

2004

A&A

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Abstract.We report new photometry of CG Cyg from [1998][1999][2000][2001][2002]. We also analyze published photometry collected since 1965. An O-C analysis reveals evidence of a third body in the system having a 51 year orbital period. After removing the effects of the third body, we note a remaining 22.5 year cyclic variation in the O-C curve that is similar to the period of the luminosity variations. Modeling the spot activity for 28 V band light curves obtained between 1965 and 2002 confirms the presence of two active longitude belts (ALBs) at approximately 90 • and 270 • . Most of the spots occur at mid latitudes with a few at low latitudes. We note no spots at latitudes greater than 60 • .

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Section: Eclipse Timings and Period Studysupporting

confidence: 72%

Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Long-term luminosity variations and period changes in CG Cygni

Afşar¹,

Heckert²,

İbanoǧlu³

2004

A&A

View full text Add to dashboard Cite

show abstract

“…The observations since that time (Yu 1923;Milone et al 1979;Jassur 1980;Sowell et al 1987;Naftilan et al 1987;Bedford et al 1987;Dapergolas et al 1989aDapergolas et al , 1994Zeilik et al 1989Zeilik et al , 1991 …”

Section: Introductionmentioning

confidence: 99%

Spectroscopic and photometric observations of the short-period RS CVn-type star CG Cyg

Kjurkchieva

Marchev

Ogłoza

2003

A&A

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Abstract. Spectroscopic observations around the H α line and BVR photometry of the eclipsing short-period RS CVn-star CG Cyg are presented. The solutions of the radial velocity curves and the light curves yielded the following masses and radii of the star components:The measured rotational broadenings of the observed lines correspond to equatorial velocities V 1 = 80 km s −1 and V 2 = 66 km s −1 . The distortions of our multicolor light curve were reproduced by two cool spots on the primary star. The strong absorption feature between the spectral lines of the two stars was explained by extended structure around the mass center of the system. The H α emission line of the secondary star in the August spectra was attributed to a prolonged flare of this star.

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Orbital Period Changes and Long Term Luminosity Variation in Active Binary CG Cyg

Jassur

Kermani

Gozaliasl

Close Binaries in the 21st Century: New Opportunities and Challenges

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Recent photometry of CG Cygni

Cited by 10 publications

References 0 publications

Long-term luminosity variations and period changes in CG Cygni

Long-term luminosity variations and period changes in CG Cygni

Spectroscopic and photometric observations of the short-period RS CVn-type star CG Cyg

Orbital Period Changes and Long Term Luminosity Variation in Active Binary CG Cyg

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