Photometric study of the short-period RS Canum Venaticorum binary RT Andromedae

Zhang, Liyun; Gu, Shenghong

doi:10.1051/0004-6361:20066767

Cited by 25 publications

(11 citation statements)

References 22 publications

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“…These active longitude features have also been found using photometry on many other active RS CVn binary systems, such as EI Eri, σ Gem, HK Lac, and RT And (Olah Hall & Henry 1991;Henry et al 1996;Berdyugina & Tuominen 1998;and Zhang & Gu 2007).…”

Section: Chromospheric Activity Modulationmentioning

confidence: 59%

Chromospheric activity on the RS Canum Venaticorum binary SZ Piscium

Zhang

Gu²

2008

A&A

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Aims. We present the new high-resolution echelle spectra of SZ Psc, obtained in Nov. 2004 and Sep.−Dec. 2006, and study its chromospheric activity. Results. All indicators show that the chromospheric activity of the system is associated with the cooler component. We find that the values of EW 8542 /EW 8498 are in the range 1−3, which indicates optically thick emission in plage-like regions. The 2006 data suggest the presence of active longitude phenomena. For the Ca ii 8542 and 8662 and the H α lines, it seems that the excess emission is stronger near the two quadratures of system. This may be anti-correlated with the behavior of the Na i D 1 line. The absorption features are detected in the subtracted H α lines, which could be explained by prominence-like extended material seen on the stellar disk or by mass transfer from the cooler component to the hotter one.

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Section: Chromospheric Activity Modulationmentioning

confidence: 59%

Chromospheric activity on the RS Canum Venaticorum binary SZ Piscium

Zhang

Gu²

2008

A&A

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“…to search the final result. The details of the procedure of photometric solution are similar to those of our previous works of RT And (Zhang & Gu 2007), DV Psc (Zhang et al 2010a), GSC 3576-0170 (Zhang et al 2010b) and KQ Gem (Zhang 2010).…”

Section: Observationsmentioning

confidence: 88%

“…As our on-going program of the study of RS CVn binary with multi-color photometry and high-resolution spectra (Gu et al 2002, Zhang & Gu 2007, Zhang & Gu 2008, Zhang et al 2010a, we present new B, V, R, and I CCD light curves of V1034 Her in two different seasons and analyze them to study the properties of active regions using the version 2003 of Wilson-Devinney code. In addition, we accumulated the maximum amplitudes of photometric distortions of short-period RS CVn binary from the literatures to discuss the relation between the photospheric starspot activity and the orbital period.…”

Section: Introductionmentioning

confidence: 99%

The new RS CVn binary V1034 Her revisited and the orbital period — activity relation of short-period RS CVn binaries using photometric distortion amplitude

Zhang¹

2012

Res. Astron. Astrophys.

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This paper presents new CCD BV RI light curves of the newly discovered RS CVn eclipsing binary V1034 Her in 2009 and 2010, which shapes are different from the previous published results. They show asymmetric outside eclipse and we try to use a spot model to explain the phenomena. Using the Wilson-Devinney program with one-spot or two-spots model, photometric solutions of the system and starspot parameters were derived. Comparing the two results, it shows that the case of two spots is better successful in reproducing the light-curve distortions. For all the spot longitudes, it suggests that the trend towards active longitude belts and each active longitude belts might be switch. Comparing the light curves of 2009 and 2010, it indicates that the light curve changes on a long time scale of one year, especially in phase 0.25. In addition, we also collected the values of the maximum amplitudes of photometric distortion of the short-period RS CVn binary. We found for the first time that there is a trend of increasing activity with decreasing the orbital period. Finally, fitting all available light minimum times including our newly obtained ones with polynomial function confirmed that the orbital period of V1034 underwent up increase.

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“…The light contribution of the optical companion is found to be 12.3%, 14.9%, 16.5% and 17.0% for the B, V, Rand I bands, respectively. The procedures for calculating the orbital and starspot parameters are similar to those in previous works on RT And (Zhang & Gu 2007) and DV Psc . Since it is difficult to obtain the starspot latitude by photometric observation, we assumed its latitude to be 90°.…”

Section: Photometric Analysesmentioning

confidence: 99%

Magnetic Activity and Period Variation Studies of the Short-period Eclipsing Binaries. II. V1101 Her, AD Phe, and NSV 455 (J011636.15–394955.7)

Zhang

et al. 2017

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In this paper, we present new BVRI light curves of short-period contact eclipsing binaries V1101 Her and AD Phe from our observations carried out from 2014 to 2015 using the SARA KP and SARA CT telescopes. There is an eclipsing binary located at α(2000)=01 h 16 m 36 15 and δ(2000)=−39°49′55 7 in the field of view of AD Phe. We derived an updated ephemeris and found there a cyclic variation overlaying a continuous period increase (V1101 Her) and decrease (AD Phe). This kind of cyclic variation may be attributed to the light time effect via the presence of the third body or magnetic activity cycle. The orbital period increase suggests that V1101 Her is undergoing a mass-transfer from the primary to the secondary component (dM 1 /dt=2.64(±0.11)×10−6 M e yr −1) with the third body (P 3 =13.9(±1.9) years), or 2.81(±0.07)×10−6 M e yr −1 for an increase andmagnetic cycle (12.4(±0.5) years). The long-term period decrease suggests that AD Phe is undergoing a mass-transfer from the secondary component to the primary component at a rate of −8.04(±0.09)×10 −8 M e yr −1 for a period decrease and the third body (P 3 =56.2(±0.8) years), or −7.11(±0.04)×10 −8 M e yr −1 for a decrease and magnetic cycle (50.3(±0.5) years). We determined their orbital and geometrical parameters. For AD Phe, we simultaneously analyzed our BVRI light curves and the spectroscopic observations obtained by Duerbeck & Rucinski. The spectral type of V1101 Her was classified as G0±2V by LAMOST stellar spectra survey. The asymmetry of the R-band light curve of AD Phe obtained by McFarlane & Hilditch in 1987 is explained by a cool spot on the primary component.

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Photometric study of the short-period RS Canum Venaticorum binary RT Andromedae

Cited by 25 publications

References 22 publications

Chromospheric activity on the RS Canum Venaticorum binary SZ Piscium

Chromospheric activity on the RS Canum Venaticorum binary SZ Piscium

The new RS CVn binary V1034 Her revisited and the orbital period — activity relation of short-period RS CVn binaries using photometric distortion amplitude

Magnetic Activity and Period Variation Studies of the Short-period Eclipsing Binaries. II. V1101 Her, AD Phe, and NSV 455 (J011636.15–394955.7)

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