Peremennye Zvezdy

"Peremennye Zvezdy",
Prilozhenie
,
vol. 7, N 2 (2007)

New RS CVn Stars. II.

I. Sergey
Belarus, Molodechno

Received:   1.01.2007;   accepted:   26.01.2007
(E-mail for contact: seriv76@tut.by)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 TYC 02879 01199 104 26 37.40 +38 45 02.3RS10.7010.85R2.09782451580.66maxG5VComm. 11.gifchart1.jpgNSVS 4325862
2 GSC 0815-0092509 03 47.71 +12 18 26.1RS12.0012.23R5.32872451601.70max Comm. 22.gifchart2.jpgNSVS 10165666
3 TYC 03009 00882 110 53 05.04 +38 13 34.2RS10.3510.48R9.77332451550.86max Comm. 33.gifchart3.jpgNSVS 4959248
4 TYC 03046 00605 114 49 52.59 +42 06 26.8RS10.8110.96R13.71372451611.88max Comm. 44.gifchart4.jpgNSVS 5151060
5 TYC 00924 00262 114 55 01.95 +14 42 03.1E/RS11.1911.42R1.74672451335.57max Comm. 55.gifchart5.jpgNSVS 10557447
6 TYC 03133 01231 119 13 02.63 +44 36 15.8RS10.2210.40R3.56572451361.75max Comm. 66.gifchart6.jpgNSVS 5529001
7 TYC 03141 02210 119 51 24.80 +40 44 07.4RS8.368.57R4.1648:2451443.78maxG5Comm. 77.gifchart7.jpgNSVS 5693987
8 TYC 03179 01343 120 52 58.27 +44 07 19.9RS10.4710.62R7.16632451415.88maxG5VComm. 88.gifchart8.jpgNSVS 5760115

Comments:


1. HDE 279788 = BD+38 891 = 1RXS J042638.5+384458. The star's spectroscopy was reported by Li & Hu (1998). From its spectrum, this can be a weak-lined T Tauri star.

2. 1RXS J090347.3+121837.

3. BD+38 2188 = 1RXS J105305.8+381333.

4. 1RXS J144952.3+420615.

5. 1RXS J145502.5+144210. A twice longer period (3.4906 days) with an EB-like phased light curve is possible.

6. 1RXS J191302.4+443629.

7. HD 226195 = BD+40 3908 = 1RXS J195125.1+404405. The period reported is only one of several possibilities.

8. BD+43 3754 = 1RXS J205257.8+440716.

Remarks:
We report variability discovery for eight stars found in the public data release from the Northern Sky Variablity Survey (NSVS; Wozniak et al., 2004; see also http://skydot.lanl/gov/nsvs). A periodicity test was performed using the Lafler - Kinman algorithm implemented in the Peranso software (Husar, 2006).

Acknowlegdements: I would like to thank Dr. Y. Beletsky for his assistance.

References:
Husar, D., 2006, BAV Rundbrief, 55, 32
Li, J.Z., Hu, J.Y., 1998, Astronomy & Astrophysics Supplement, 132, 173
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436



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