Peremennye Zvezdy

"Peremennye Zvezdy",
Prilozhenie
,
vol. 10, N 27 (2010)

New RS CVn Variables in the NSV Catalogue

K. Bernhard#1,2, S. Otero#3
#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

Received:   7.09.2010;   accepted:   3.11.2010
(E-mail for contact: klaus.bernhard@liwest.at)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1NSV 15584GSC 07018-0050702 48 07.93, -36 58 53.7RS7.837.88V17.6982452710.52minG1VComm. 1NSV_15584.jpg NSV_15584
2NSV 16633GSC 07056-0134205 40 49.00, -31 24 06.9RS8.628.80V9.162451868.70minG7IIIComm. 2NSV_16633.jpg NSV_16633
3NSV 16803GSC 07084-0109806 12 43.58, -36 37 55.2RS8.158.22V10.3052454890.60minK0IIIComm. 3NSV_16803.jpg NSV_16803
4NSV 3374GSC 01345-0006307 05 47.61, +15 01 21.4RS9.379.46V35.532454524.55minG5VComm. 4NSV_3374.jpg NSV_3374
5NSV 18506GSC 08210-0022610 44 47.89, -50 53 06.2RS7.768.03V65.532453109.71minG6IIIComm. 5NSV_18506.jpg NSV_18506
6NSV 6937GSC 05580-0050315 06 44.49, -08 38 48.1RS10.9311.14V18.732453062.80minG8Comm. 6NSV_6937.jpg NSV 6937
7NSV 20419GSC 08697-0146615 52 38.45, -53 26 15.0RS7.908.24V99.12452667.86minG8IIIComm. 7NSV_20419.jpg NSV_20419
8NSV 20781GSC 07371-0023616 49 44.55, -36 24 22.2RS8.068.41V31.222454521.84minG7IIIComm. 8NSV_20781.jpg NSV_20781
9NSV 14697GSC 07521-0093623 46 03.13, -35 35 20.6RS10.5810.74V20.982455144.65minG7IVComm. 9NSV_14697.jpg NSV_14697

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:
Høg, E., Fabricius, C., Makarov, V.V., et al., 2000, Astron. Astrophys., 355, L27
Houk, N., Cowley, A.P., 1975, University of Michigan Catalogue of two-dimensional spectral types for the HD stars, Ann Arbor, Dep. of Astron., Univ. of Michigan
Koen, C., Eyer, L., 2002, Monthly Notices of the Royal Astron. Soc., 331, 45
Lenz, P., Breger, M., 2005, Comm. in Asteroseismology, 146, 53
Nassau, J.J., MacRae, D.A, 1955, Astrophys. J., 121, 32
Olsen, E.H., 1980, IBVS, No. 1770
Olsen, E.H., 1993, Astron. Astrophys. Suppl. Ser., 102, 89
Pojmanski, G., 2002, Acta Astronomica, 52, 397
Röser, S., Schilbach, E., Schwan, H., et al., 2008, Astron. Astrophys., 488, 401
Skrutskie, M.F., Cutri, R.M., Stiening, R., et al., 2006, Astron. J., 131, 1163
Torres, C.A.O., Quast, G.R., da Silva, L., et al., 2006, Astron. Astrophys., 460, 695
Voges, W., Aschenbach, B., Boller, Th., et al., 1999, Astron. Astrophys., 349, 389
Voges, W., Aschenbach, B., Boller, T., et al., 2000, IAU Circ., No. 7432



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