Peremennye Zvezdy (Variable Stars) 35, No. 5, 2015
Received 3 December; accepted 11 December.
A. V. Khruslov
Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia; e-mail: email@example.com
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RRC stars with a single non-radial pulsation whose frequency is close to that of the first overtone were first discovered by Olech et al. (1999) in the globular cluster M55 (three variables). Alcock et al. (2000) identified 24 such stars among variables in the Large Magellanic Cloud (the MACHO project; the variability type designated RR1-1). A star of this kind, TYC 6556 00609 1, is known in the galactic field (Antipin & Jurcsik 2005). Later, I detected two variables of this type: GSC 2493-00118 and USNO-A2.0 0900-20281750 (Khruslov 2012).
The period ratios for stars of this type (assuming , although it is possible that ) are within 0.9-0.999. The amplitude of the non-radial oscillation can be considerably lower than the amplitude of the main one, but these amplitudes can also be virtually the same.
In this article, I present a discovery of 14 new cases of RRC stars with a single excited additional non-radial mode. These stars were found in the our search for RR Lyrae variables with two radial pulsations, F/1O (Khruslov 2014, 2015ab). The variability of all these variables was announced by Drake et al. (2014) in the Catalina Surveys Periodic Variable Star Catalog. One variable (No. 2) was classified as a double-mode RR Lyrae star, type RR(B) in GCVS classification (Samus et al. 2007-2015); 13 other variables were classified as single-mode first-overtone RR Lyrae star (type RRC). There are two cases of wrong periods announced in the Catalina surveys periodic variable star catalog: Nos. 5 and 10, with periods being one-day aliases of the real first overtone period.
Information on the studied stars is presented in Tables 1 and 2. Finding charts and data are available online in the html version of this paper as a zip-archive. The light curves of all the stars displayed in Figs. 1 and 2.
The star designations are from the USNO-B1.0 catalog (Monet et al. 2003). The tabulated coordinates of the variables were drawn either from the GSC2.3 (Lasker et al. 2008) or from the 2MASS (Skrutskie et al. 2006) catalogs.
Table 1 contains, for each star, its equatorial coordinates (J2000); number from the USNO-B1.0 catalog; magnitudes in maximum and minimum in the Catalina surveys photometric system; period previously known for the star, according to the Catalina surveys periodic variable star catalog.
|No.||Coordinates (J2000)||USNO-B1.0||Magn.||, days|
|1||02343944 +045528 4||0949-0024801||1384-1426||0.281675|
|2||08 25 19.75 +37 48 25.0||1278-0205991||15.12-15.45||0.2563464|
|3||10 19 59.98 +30 17 54.6||1202-0180839||17.6-18.3||0.3093978|
|4||10 24 22.39 +36 55 24.3||1269-0201347||13.95-14.37||0.3066193|
|5||12 11 43.61 -16 45 00.8||0732-0287960||15.79-16.39||0.3678677|
|6||12 32 04.84 +18 20 09.7||1083-0224291||15.82-16.29||0.263563|
|7||14 11 13.47 +06 40 13.7||0966-0241897||15.84-16.25||0.2772159|
|8||14 16 04.81 +29 59 08.3||1199-0219251||15.76-16.11||0.2940443|
|9||14 34 29.84 +26 57 28.0||1169-0257343||16.11-16.48||0.2696107|
|10||15 07 36.04 +10 05 02.6||1000-0239484||17.03-17.76||0.4735085|
|11||16 31 59.91 +33 51 35.3||1238-0254586||16.65-17.30||0.2744261|
|12||17 40 16.19 +31 59 50.5||1219-0309843||15.65-16.14||0.3475867|
|13||23 18 25.66 +24 25 51.8||1144-0564929||15.31-15.87||0.3054350|
|14||23 57 56.77 +29 17 34.0||1192-0600617||16.55-17.26||0.299204|
Table 2 presents light elements and amplitudes of two oscillations: the first-overtone period ; the non-radial-mode period ; the first-overtone and non-radial mode epochs of maxima (expressed as JD - 2455000); period ratio ; beat period (or Blazhko effect period); semi-amplitudes of first-overtone () and non-radial-mode () oscillations. Additional information about some of the stars is collected in Remarks.
|No.||, d||, d||Epoch||Epoch|
1. GSC 0049-00915.
4. GSC 2517-00730. The SWASP data were additionally used. From 1SWASP data, 136-1437, , .
11. Two entries with identical coordinates in the Catalina surveys periodic variable star catalog (Drake et al. 2014). The period is given for the second entry.
12. The star has a faint close red companion 2MASS 17401606+3159476, . The variable is much brighter than the red companion in the band; the components are of comparable brightness in the POSS IR band.
13. There is a possible second non-radial pulsation, with the period and amplitude .
The periods of dominant oscillations (first overtone, ) for all our stars are within 0.256-0.348 days. As for periods of the non-radial modes, the and cases are equally frequent. The period ratios for these stars are within 0.964-0.999 and 1.003-1.026. The beat periods (Blazhko effect periods) are from 8.2 to 231 days. The amplitude ratios are within 1.03-3.57.
Acknowledgments: The author wishes to thank Dr. V.P. Goranskij for providing his software. This study was supported by the Russian Foundation for Basic Research (grant 13-02-00664) and by the Programme "Non-stationary Phenomena of Objects in the Universe" of the Presidium of Russian Academy of Sciences.
Fig. 1. The light curves of the stars Nos. 1-7. The left panel present data folded with the first overtone periods. The central and right panels show the same curves after prewhitening the other oscillation (frequencies and ).
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