Peremennye Zvezdy

Article in PDF
"Peremennye Zvezdy",
Prilozhenie
,
vol. 12, N 25 (2012)

Seven Double-Mode RR Lyrae Variables

A. V. Khruslov
Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

ISSN 2221–0474

Received:   5.12.2012;   accepted:   27.12.2012
(E-mail for contact: khruslov@bk.ru)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 USNO-A2.0 0900-0670509410 30 08.33, +03 36 08.4RR(B)15.1215.70CV(see Comments)(see Comments)max Comm. 11.PNGchart1.PNGCSS_data_1.txt
2 USNO-A2.0 0900-0690714811 21 05.14, +03 30 56.0RR(B)16.6417.45CV(see Comments)(see Comments)max Comm. 22.PNGchart2.PNGCSS_data_2.txt
3 GSC 0293-0105212 49 28.95, +03 22 41.6RR(B)14.6815.26CV(see Comments)(see Comments)max Comm. 33.PNGchart3.PNGCSS_data_3.txt
4 GSC 0310-0092213 31 16.06, +03 34 07.4RR(B)13.6814.46CV(see Comments)(see Comments)max Comm. 44.PNGchart4.PNGCSS_data_4.txt
5 GSC 0321-0087214 20 22.40, +03 06 51.9RR(B)14.2914.94CV(see Comments)(see Comments)max Comm. 55.PNGchart5.PNGCSS_data_5.txt
6 USNO-A2.0 0900-0846879416 11 04.26, +03 28 52.9RR(B)16.5817.29CV(see Comments)(see Comments)max Comm. 66.PNGchart6.PNGCSS_data_6.txt
7V2220 SgrGSC 7959-0172520 00 22.55, -44 31 01.7RR(B)15.316.8SWASP(see Comments)(see Comments)max Comm. 77.PNGchart7.PNG1SWASP_data_7.txt

Comments:


1. The variability of USNO-A2.0 0900-06705094 was discovered by Kraus et al. (2007, MG1 646352), log P = 0.153. The AAVSO Variable Star Index (VSX; www.aavso.org/vsx/) suggests type RRC, without light elements. According to data from Catalina Surveys, it is actually a double-mode RR Lyrae star, type RR(B), with the light elements tabulated below.

ModeFrequency, c/d Semi-amplitude, SV mag Period, days Epoch, JD
f1 2.301936 0.155 0.434417 2454800.820
f0 1.720318 0.053 0.581288 2454801.000
f1 + f0 4.022186 0.022 0.248621 2454800.608
f1 – f0 0.581649 0.021 1.71925 2454801.90

P1/P0 = 0.7473. J – K = 0.362 (2MASS).

2. The variability of USNO-A2.0 0900-06907148 was discovered by Kraus et al. (2007, MG1 666086), log P = 0.65. The AAVSO Variable Star Index suggests type RRC, without light elements. According to data from Catalina Surveys, it is actually a double-mode RR Lyrae star, type RR(B), with the light elements tabulated below.

ModeFrequency, c/d Semi-amplitude, SV mag Period, days Epoch, JD
f1 2.781804 0.151 0.359479 2454800.634
f0 2.069973 0.105 0.483098 2454800.541
f1 + f0 4.85178 0.049 0.206110 2454800.574

P1/P0 = 0.7441. J – K = 0.203 (2MASS).

3. The variability of GSC 0293-01052 was discovered by Kraus et al. (2007, MG1 698628), log P = 0.3. The AAVSO Variable Star Index suggests type RRAB, without light elements. According to data from Catalina Surveys, it is actually a double-mode RR Lyrae star, type RR(B), with the light elements tabulated below.

ModeFrequency, c/d Semi-amplitude, SV mag Period, days Epoch, JD
f1 2.558644 0.163 0.390832 2454800.880
f0 1.906836 0.095 0.524429 2454800.650

P1/P0 = 0.7453. J – K = 0.265 (2MASS).

4. The variability of GSC 0310-00922 was discovered by Kraus et al. (2007, MG1 716004), log P = 2.474. The AAVSO Variable Star Index suggests type RRAB, without light elements. According to data from Catalina Surveys, it is actually a double-mode RR Lyrae star, type RR(B), with the light elements tabulated below.

ModeFrequency, c/d Semi-amplitude, SV mag Period, days Epoch, JD
f1 2.953372 0.149 0.338596 2454800.060
f0 2.193093 0.142 0.455977 2454800.145
f1 + f0 5.14655 0.047 0.194305 2454800.070
f1 – f0 0.760375 0.038 1.31514 2454801.05

P1/P0 = 0.7426. J – K = 0.255 (2MASS).

5. The variability of GSC 0321-00872 was discovered by Kraus et al. (2007, MG1 738552), log P = 2.874. The AAVSO Variable Star Index suggests type RRAB, without light elements. According to data from Catalina Surveys, it is actually a double-mode RR Lyrae star, type RR(B), with the light elements tabulated below.

ModeFrequency, c/d Semi-amplitude, SV mag Period, days Epoch, JD
f1 2.653780 0.150 0.376821 2454800.570
f0 1.976957 0.089 0.505828 2454800.750
f1 + f0 4.630744 0.032 0.215948 2454800.627
f1 – f0 0.676773 0.027 1.47760 2454801.40

P1/P0 = 0.7450. J – K = 0.132 (2MASS).

6. The variability of USNO-A2.0 0900-08468794 was discovered by Kraus et al. (2007, MG1 816948), log P = 2.449. The AAVSO Variable Star Index suggests type RRC, without light elements. According to data from Catalina Surveys, it is actually a double-mode RR Lyrae star, type RR(B), with the light elements tabulated below.

ModeFrequency, c/d Semi-amplitude, SV mag Period, days Epoch, JD
f1 2.803500 0.177 0.356697 2454800.751
f0 2.087055 0.065 0.479144 2454800.609

P1/P0 = 0.7444.

7. The variability of V2220 Sgr was discovered by Hoffmeister (1963). The variable is listed in the GCVS as an RR star without light elements. According to data from SuperWASP, it is actually a double-mode RR Lyrae star, type RR(B), with the light elements tabulated below.

ModeFrequency, c/d Semi-amplitude, mag Period, days Epoch, JD
f1 2.51345 0.341 0.39786 2454300.879
f0 1.87434 0.184 0.53352 2454300.810
f1 + f0 4.38781 0.087 0.227904 2454300.825
f1 – f0 0.63902 0.080 1.5649 2454301.06

P1/P0 = 0.7457. J – K = 0.184 (2MASS). When plotting the phased light curves for the identified frequencies, f1 and f0, I also subtracted variations of the mean brightness in the 1SWASP data, probably of instrumental origin (corresponding to the frequency f = 1 in the power spectra).

Remarks:
I present a new investigation of seven known RR Lyrae variable stars. I analyzed all observations available for these stars in the Catalina Surveys (Drake et al. 2009) and SuperWASP (Butters et al. 2010) online public archives using the period-search software developed by Dr. V.P. Goranskij for Windows environment. According to these data, the variables are double-mode RR Lyrae variables, pulsating in the first-overtone and fundamental modes.

Their period ratios, P1/P0, are typical of radially pulsating double-mode RR Lyrae stars. Along with the light curves, I present power spectra of the RR Lyrae variables, for the raw data and after subtraction of the first-overtone oscillations. The structure of the power spectra shows that the secondary periods are real.

The SuperWASP observations are available as FITS tables which were converted into ASCII tables using the OMC2ASCII program as described by Sokolovsky (2007). When reducing the SuperWASP observations, I rejected nights with large scatter of data points, probably due to weather or instrumental errors.

The tabulated coordinates of the variables were drawn either from the 2MASS catalog or from the GCVS (Samus et al. 2007–2012).

Acknowledgements: Thanks are due to Dr. K.V. Sokolovsky for his advice concerning data retrieving. The author wishes to thank Dr. V.P. Goranskij for providing his software. I am grateful to Dr. A.L. Kraus for providing access to the MG1 Variable Star Catalog (MG1-VSC).

References:
Butters, O.W., West, R.G., Anderson, D.R., et al., 2010, Astron. Astrophys., 520, L10
Drake, A.J., Djorgovski, S.G., Mahabal, A., et al., 2009, Astrophys. J., 696, 870
Hoffmeister, C., 1963, Veröff. Sternwarte Sonn., 6, 1
Kraus, A.L., Craine, E.R., Giampapa, M.S., et al.,2007, Astron. J., 134, 1488
Samus, N.N., Durlevich, O.V., Kazarovets, E V., et al., 2007–2012, General Catalogue of Variable Stars, Centre de Donnees Astronomiques de Strasbourg, B/gcvs
Sokolovsky, K.V., 2007, Perem. Zvezdy Prilozh., 7, No. 30



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