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"Peremennye Zvezdy", Prilozhenie, vol. 10, N 27 (2010) |
#1. Linz, Austria;
#2. Bundesdeutsche Arbeitsgemeinschaft fuer Veraenderliche Sterne e.V. (BAV), Berlin, Germany; #3. Asociación Cielo Sur Grupo Wezen 1 88, Buenos Aires, Argentina |
ISSN 2221–0474 |
Received: 7.09.2010; accepted: 3.11.2010
(E-mail for contact: klaus.bernhard@liwest.at)
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Comments:
1. Johnson B-V = 0.609 (derived from Tycho-2); J-K = 0.507 (2MASS).
Proper motion: pmRA = 21.71 mas/yr, pmDE = 33.05 mas/yr (Röser et al. 2008).
ROSAT: 1RXS J024807.9-365857; HR1 = -0.10, HR2 = 0.39.
Spectral type: G1V, EW(Li) = 0 (Torres et al. 2006).
Known visual binary star (Olsen 1980).
2. Johnson B-V = 1.089 (derived from Tycho-2); J-K = 0.741 (2MASS).
Proper motion: pmRA = 12.52 mas/yr, pmDE = -25.88 mas/yr (Röser et al. 2008).
ROSAT: 1RXS J054048.7-312402; HR1 = 0.19, HR2 = 0.33.
Spectral type: G7III, EW(Li) = 0 (Torres et al. 2006).
3. Johnson B-V = 0.952 (derived from Tycho-2); J-K = 0.634 (2MASS).
Proper motion: pmRA = -7.25 mas/yr, pmDE = -2.85 mas/yr (Röser et al. 2008).
ROSAT: 1RXS J061243.3-363755, HR1 = 0.28, HR2 = 0.22.
Spectral type: K0III spec bin, EW(Li) = 90 (Torres et al. 2006).
Type RS: (Olsen 1993).
4. Johnson B-V = 1.109 (derived from Tycho-2); J-K = 0.689 (2MASS).
Proper motion: pmRA = 2.06 mas/yr, pmDE = -3.49 mas/yr (Röser et al. 2008).
ROSAT: 2RXP J070547.1+150130, HR1 = 0.44, HR2 = 0.04.
Spectral type: G5V (Nassau & MacRae 1955).
5. Johnson B-V = 0.836 (derived from Tycho-2); J-K = 0.611 (2MASS).
Proper motion: pmRA = -44.94 mas/yr, pmDE = 5.27 mas/yr (Röser et al. 2008).
ROSAT: 1RXS J104447.7-505310, HR1 = 0.45, HR2 = 0.35.
Spectral type: G6III, SB2, EW(Li) = 30 (Torres et al. 2006).
6. Johnson B-V = 0.879 (derived from Tycho-2); J-K = 0.737 (2MASS).
Proper motion: pmRA = 13.95 mas/yr, pmDE = -3.93 mas/yr (Röser et al. 2008).
Spectral type: G8 (GCVS, NSV).
7. Johnson B-V = 1.155 (derived from Tycho-2); J-K = 0.787 (2MASS).
Proper motion: pmRA = -6.46 mas/yr, pmDE = -4.53 mas/yr (Röser et al. 2008).
ROSAT: 1RXS-F J155238.4-532603, HR1 = 1.00, HR2 = 0.19.
Spectral type: G8III (Houk & Cowley 1975).
8. The star HIP 82360 (= NSV 20781) is mentioned by Koen & Eyer (2002) as a variable with variation frequency equivalent to the period of 31.53 days.
Johnson B-V = 1.013 (derived from Tycho-2); J-K = 0.714 (2MASS).
Proper motion: pmRA = 27.31 mas/yr, pmDE = -12.28 mas/yr (Röser et al. 2008).
ROSAT: 1RXS J164944.7-362421, HR1 = 1.00, HR2 = 0.29.
Spectral type: G7III, EW(Li) = 0 (Torres et al. 2006).
9. Johnson B-V = 0.715 (derived from Tycho-2); J-K = 0.656 (2MASS).
Proper motion: pmRA = 71.66 mas/yr, pmDE = -22.29 mas/yr (Röser et al. 2008).
ROSAT: 1RXS J234604.8-353541, HR1 = 0.08, HR2 = 0.61.
Spectral type: G7IV, EW(Li) = 70 (Torres et al. 2006).Remarks:
Nine new RS CVn variables were found by the investigation of ASAS-3 (http://www.astrouw.edu.pl/asas/?page=main, Pojmanski 2002) light curves of objects listed in the New Catalogue of Suspected Variable Stars (NSV, http://www.sai.msu.su/gcvs/gcvs/new.htm).
Each object was checked against the Strasbourg CDS Vizier service and the International Variable Star Index (http://www.aavso.org/vsx/) for pre-existence as a chromospherically active star in variability catalogues.
The criteria for including a star in this list of RS CVn stars after an analysis of the available data with Period 04 (Lenz and Breger 2005) were:
i) period, amplitude and shape of the light curve are consistent with the definition of RS CVn in the GCVS,
ii) appropriate spectral types, 2MASS J-K (Skrutskie et al. 2006) and B-V (Høg et al. 2000) colour indices,
iii) the X-ray identifications (Voges et al. 1999; Voges et al. 2000),
iiii) further information like the lithium content as indicator of young stellar objects and proper motions.
Some of these RS CVn stars showed a clear variation of the shape of the light curves. For these objects the ephemeris and the folded light curves are given for a distinct period of time (described in figure as HJD 245....-....). This is somewhat typical of chromospherically active stars which can show secular variation in mean magnitude and/or amplitude as a result of starspot cycles similar in nature to the Suns`s sunspot cycle.
Besides the nine stars in the Table, we also analyzed the GCVS star HL Leo (the GCVS type BY, P = 37.17 days). We find a different period in the ASAS-3 data (P = 31.89 days). In our opinion, this is also an RS CVn variable, in agreement with its spectral type G2IV or G2III in several sources as well as with the Hipparcos parallax indicating a subgiant or giant luminosity.
Acknowledgements: This research has made use of the SIMBAD and VizieR databases operated at the Centre de Données Astronomiques (Strasbourg) in France, of the Smithsonian/NASA Astrophysics Data System, of the International Variable Star Index (AAVSO) and of the Two Micron All Sky Survey. It is a pleasure to thank John Greaves, UK for his suggestions and helpful comments. We would like to thank S.V. Antipin and N.N. Samus for helpful discussion and for improving the paper.References:
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