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Long-term magnetic activity in close binary systems. I. Patterns of color variations
Aims.This is the first of a series of papers in which we present theresults of a long-term photometric monitoring project carried out atCatania Astrophysical Observatory aimed at studying magnetic activity inlate-type components of close binary systems, its dependence on globalstellar parameters, and its evolution on different time scales from daysto years. In this first paper, we present the complete observationdataset and new results of an investigation into the origin ofbrightness and color variations observed in the well-known magneticallyactive close binary stars: AR Psc, VYAri, UX Ari, V711 Tau,EI Eri, V1149 Ori, DHLeo, HU Vir, RS CVn,V775 Her, AR Lac, SZPsc, II Peg and BY Dra Methods: About 38 000 high-precision photoelectric nightly observationsin the U, B and V filters are analysed. Correlation and regressionanalyses of the V magnitude vs. U-B and B-V color variations are carriedout and a comparison with model variations for a grid of active regiontemperature and filling factor values is also performed. Results: Wefind the existence of two different patterns of color variation. Eightstars in our sample: BY Dra, VYAri, V775 Her, II Peg,V1149 Ori, HU Vir, EIEri and DH Leo become redder when theybecome fainter, as is expected from the presence of active regionsconsisting of cool spots. The other six stars show the oppositebehaviour, i.e. they become bluer when they become fainter. ForV711 Tau this behaviour could be explained by theincreased relative U- and B-flux contribution by the earlier-typecomponent of the binary system when the cooler component becomesfainter. On the other hand, for AR Psc, UXAri, RS CVn, SZ Psc andAR Lac the existence of hot photospheric faculae mustbe invoked. We also found that in single-lined and double-lined binarystars in which the fainter component is inactive or much less active theV magnitude is correlated to B-V and U-B color variations in more than60% of observation seasons. The correlation is found in less than 40% ofobservation seasons when the fainter component has a non-negligiblelevel of activity and/or hot faculae are present but they are eitherspatially or temporally uncorrelated to spots.I dedicate this paper to the memory of the P.I. of this project, Prof.Marcello Rodonò, who suddenly passed away on October 23, 2005. Tohim my sincere estimation and deepest gratitude.Based onobservations collected at INAF-Catania Astrophysical Observatory, Italy.
| The N2K Consortium. VII. Atmospheric Parameters of 1907 Metal-rich Stars: Finding Planet-Search Targets
We report high-precision atmospheric parameters for 1907 stars in theN2K low-resolution spectroscopic survey, designed to identify metal-richFGK dwarfs likely to harbor detectable planets. Of these stars, 284 arein the ideal temperature range for planet searches,Teff<=6000 K, and have a 10% or greater probability ofhosting planets based on their metallicities. The stars in thelow-resolution spectroscopic survey should eventually yield >60 newplanets, including 8-9 hot Jupiters. Short-period planets have alreadybeen discovered orbiting the survey targets HIP 14810 and HD 149143.
| UBV observations of RS Canum Venaticorum
Photoelectric observations of eclipsing binary RS CVn were carried outat Uttar Pradesh State Observatory in Nainital, India. The light curveshows wave-like distortion. Colors and magnitudes of RS CVn andcomparison stars BD + 35 deg 2421 and BD + 35 deg 2422 have been given.
| Photoelectric observations and the wave minimum of RS CVn
B, V observations of the eclipsing binary RS CVn have been presented. Adip around 0.1 p appears to be a wave minimum which fits well in the'wave minimum phase-time' relation, but deviates from the 'waveamplitude-time' relation, derived for the RS CVn. Either, the 'waveamplitude-time' relation requires a modification, or the amplitude ofthe wave minimum appears masked by the intrinsic variability of one ofthe components or by the sun-spot activity of the system. The colorexhibits variation. The secondary component appears active.
| Sulle variazioni della curva di luce del sistema RS CVn
Not Available
| A Photoelectric Study of the Eclipsing Stars RS Canum Venaticorum and YY Sagittarii.
Abstract image available at:http://adsabs.harvard.edu/abs/1951ApJ...113..637K
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| Takýmyýldýz: | Av Kopekleri |
| Sað Açýklýk: | 13h12m49.22s |
| Yükselim: | +34°53'19.0" |
| Görünürdeki Parlaklýk: | 8.524 |
| Uzaklýk: | 63.613 parsek |
| özdevim Sað Açýklýk: | -21.2 |
| özdevim Yükselim: | 48 |
| B-T magnitude: | 9.235 |
| V-T magnitude: | 8.583 |
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