Peremennye Zvezdy

"Peremennye Zvezdy",
Prilozhenie
,
vol. 7, N 21 (2007)

New RS CVn Stars without Eclipses II

A. V. Khruslov
Russia, Tula

Received:   15.08.2007;   accepted:   11.10.2007
(E-mail for contact: khruslov@bk.ru)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 TYC 2323 00569 102 25 29.15, +30 41 50.5RS11.311.6R5.0952451501.75max Comm. 11.PNGchart1.PNGNSVS 6526224 NSVS 6555193
2 TYC 2906 01122 104 56 39.17, +43 48 46.0RS9.69.9R52.2451500.0max Comm. 22.PNGchart2.PNGNSVS 4358805
3 GSC 3035-0017714 25 10.30, +39 20 00.6RS12.713.0R6.3722451388.75max Comm. 33.PNGchart3.PNGNSVS 5103437 NSVS 7751118
4 GSC 3473-0017414 32 41.24, +46 11 39.9RS12.0912.24R6.8622451411.68max Comm. 44.PNGchart4.PNGNSVS 5122418 NSVS 5129022
5 TYC 3486 00678 115 39 20.87, +47 45 23.9RS10.9511.25R20.02451395.5max Comm. 55.PNGchart5.PNGNSVS 5190120 NSVS 5199439
6 GSC 3057-0174215 57 49.58, +41 23 19.8RS12.8213.13R15.92451393.0max Comm. 66.PNGchart6.PNGNSVS 5226603
7 GSC 3064-0071116 06 50.60, +41 17 34.9RS12.913.1R0.589402451385.69max Comm. 77.PNGchart7.PNGNSVS 5231025
8 GSC 3522-0069017 47 19.65, +51 33 18.5RS14.214.7R4.2152451388.90max Comm. 88.PNGchart8.PNGNSVS 5393924

Comments:


1. X-ray source 1RXS J022526.9+304205.

2. Probably can be identified with the X-ray source 1RXS J045638.6+434820 (in 29"). B-V = 1.410 (Tycho2), J-K = 0.797 (2MASS). Types SR or CEP are not excluded. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis. The use of these data considerably increases the number of available observations without deteriorating quality and allows us to determine the period more accurately.

3. X-ray source 1RXS J142509.3+391953.

4. X-ray source 1RXS J143241.5+461132. Period P=1.1708d is not excluded.

5. X-ray source RX J1539.3+4745.

6. X-ray source 1WGA J1557.7+4123.

7. X-ray source 1RXS J160650.2+411729.

8. X-ray source 1RXS J174718.8+513310.

Remarks:
I present the discovery of 8 new RS CVn stars without eclipses. This classification is in agreement with the stars' relatively small amplitudes and with our identification of the stars with X-ray sources. A search for variables was carried out in the publicly available data of the Northern Sky Variability Survey (NSVS, Wozniak et al., 2004, also see http://skydot.lanl.gov/nsvs). These observations were analyzed using the period-search software developed by Dr. V.P. Goranskij for Windows environment. The coordinates were drawn either from the Tycho-2 or 2MASS catalogs.

References:
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436



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