The active RS Canum Venaticorum binary II Pegasi
نویسنده
چکیده
A total of 6 new surface images of II Peg obtained for the years 1997 and 1998 confirms the recently revealed permanent active longitude structure. The lower limit of the active longitudes’ lifetime is now extended up to 25 years. A new “flipflop” phenomenon, redefined as a switch of the activity between the active longitudes, has started in summer of 1998. It coincides reasonably well with the moment predicted from the activity cycle of the star. This confirms definitely the cyclic behaviour of the activity of II Peg we recently discovered. Therefore, we assign numbers to the cycles of 4.65 yr since the earliest photoelectric observations of II Peg and define the active longitudes as “odd” and “even” corresponding to odd and even numbers of cycles. With such a definition, in late 1998 the 7th cycle began and the “odd” active longitude became more active. From the analysis of the spot area evolution within the active longitudes we conclude that the activity cycle is developed as a rearrangement of the nearly constant amount of the spot area between the active longitudes. We discuss the “flip-flop” phenomenon as a tracer of stellar activity and the role of the unseen secondary in establishing the cycle.
منابع مشابه
A probable RS CVn star which sometimes stops its eclipses ⋆
We report the discovery of a new variable star, called S 10947 Aql, as the likely optical counterpart of RX J2009.8+1557. The optical variability pattern as well as the detected X-ray emission suggest that it is a chromospherically active binary of the RS Canum Venaticorum (≡ RS CVn) type. We discovered an occasional disappearance of the eclipsing minima as well as large variations in the eclip...
متن کاملThe long-period RS Canum Venaticorum binary IM Pegasi I. Orbital and stellar parameters
New high-resolution and high signal-to-noise ratio spectroscopic observations carried out in 1996–1997 are analysed. A total of 85 new high quality radial velocity measurements are used for determining the new orbital parameters: Tconj=HJD2450342.883+24.64880E, e=0.0, γ=–14.09 km s−1, K1=34.39 km s−1. A model atmosphere analysis of the averaged spectrum of the star has yielded a self-consistent...
متن کاملThe chromosphere of II Pegasi: multi-line modelling of an RS Canum Venaticorum star
We present the first simultaneous multi-line fitting of a semi-empirical atmospheric model with a chromosphere and transition region to the H I and Ca II spectra of an RS CVn star (II Peg). The static component of the Hα emission core, the line profile of Hβ, the apparent absence of Hγ and Hδ, and the emission core profiles of Ca II K and two of the Ca II IR3 lines are all approximately fitted ...
متن کاملQuiescent and Flaring Structure in Rs Canum Venaticorum Stars
Four of the most active RS CVn stars (V711 Tau, II Peg, Gem, and UX Ari) have been observed for a total of 3Ms with the Extreme Ultraviolet Explorer satellite (EUVE) between 1992 and 2000 January. Flaring and quiescent states of extreme ultraviolet spectra ( 70–740) and light curves ( 75–175) have been analyzed to provide emission measure distributions (EMD) for these systems in the range logTe...
متن کاملNear-simultaneous X-ray and optical observations of the RS Canum Venaticorum binary SV Camelopardalis
Wereport on amulti-wavelength campaign of optical and X-ray observations of the short-period eclipsing RS CVn binary star SV Cam. We present an X-ray light curve measured by ROSAT in Aug. 93, two V -band light curves obtained in Sep. and Nov. 93, and Doppler imagery based on high-resolution spectroscopy of photospheric absorption lines observed Sep.–Nov. 93. The total X-ray output of the SV Cam...
متن کامل