Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 13, N 15 (2013) |
#1. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow,
Russia;
#2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia |
ISSN 2221–0474 |
Received: 25.05.2013; accepted: 29.10.2013
(E-mail for contact: antipin@sai.msu.ru, khruslov@bk.ru)
|
Comments:
1. The variability of HH Her was discovered by Hoffmeister (1936). The variable was classified as a short-period star. Ahnert et al. (1941) classified HH Her as an RRC star with the elements: JD(max) = 2429721.650 + 0.29986×E (mag. range 15.m5 – 15.m8 pg). However, according to CSS data, the star does not vary.
2. The variability of V368 Her was discovered by Hoffmeister (1959). Following Hoffmeister (1960), the variable was classified in the GCVS as an RR Lyrae star (RRAB) with the light elements: JD(max) = 2435953.440 + 0.543689×E. This period is wrong. According to data from Catalina Surveys, the period is a little longer than one day (see Table). M – m = 0.14 P. J – K = 0.501 (2MASS).
3. The variability of V413 Her was discovered by Hoffmeister (1959), who suggested a period of 0.5137 days. Following Hoffmeister (1960), the variable was classified in the GCVS as an RR Lyrae star (RRC) with the light elements: JD(max) = 2435955.458 + 0.351742×E. These period and type are wrong. According to data from Catalina Surveys, it is an RRAB star and its variability period is close to one day. M – m = 0.15 P. J – K = 0.522 (2MASS).
4. The variability of V426 Her was discovered by Hoffmeister (1959). Following Hoffmeister (1960), the variable was classified in the GCVS as an eclipsing binary (EW/KW) with the light elements JD(min) = 2427571.460 + 0.4921282×E. According to data from Catalina Surveys, it is actually an RR Lyrae star (RRC). M – m = 0.43 P. J – K = 0.256 (2MASS).
5. The variability of V470 Her was discovered by Hoffmeister (1949). Hoffmeister (1960) found the star's Algol-like fadings and also occasional brightenings. Thus, the GCVS gives the type IS for the star (mag. range 15.m1 – 16.m0 pg). However, Ponomareva (1969) found no H-alpha emission in the spectrum. According to data from Catalina Surveys, V470 Her is actually an eclipsing binary (type EA), MinII = 15.53 (CV). D = 0.10 P.
6. The variability of V517 Her was discovered by Hoffmeister (1949), the variable was classified as a possible short-period variable. Following Hoffmeister (1960), the variable was classified in the GCVS as an RR Lyrae star with the possible light elements JD(max) = 2429022.583 + 0.597303×E. This period is not correct. According to data from Catalina Surveys, it is actually an RRAB star with P = 0.480396 days. M – m = 0.11 P. J – K = 0.326 (2MASS).
7. The variability of V541 Her was discovered by Hoffmeister (1966b), the variable was classified as an RR Lyrae variable star with undetermined light elements. Following Busch et al. (1974), the variable was classified in the GCVS as an RRAB star with the light elements JD(max) 2438503.541 + 0.568227×E. Kinemuchi et al. (2006) derived the period 0.568234 days from the NSVS data. Drake et al. (2013) give the light elements HJD(max) = 2453469.9247 + 0.5681947×E based on data from Catalina Surveys. We reinvestigated the star using the same Catalina survey data and found that the star was an RRAB variable with two closely spaced frequencies. The light elements are the following:
Mode Frequency, c/d Semi-amplitude, CV mag Period, days Epoch, JD f1 1.759913 0.374 0.568210 2454800.593 f2 1.781410 0.121 0.561353 2454800.880
f1 / f2 = 0.9879. The two close periods can also be interpreted as a Blazhko effect with the period of 46.5 days. J – K = 0.201 (2MASS).
8. The variability of V561 Her was discovered by Hoffmeister (1966a), the variable was classified in the GCVS as an RR Lyrae star without light elements. We confirm the RR Lyrae nature of this variable (RRAB type) according to data from Catalina Surveys.
M – m = 0.20 P. J – K = 0.239 (2MASS).
9. The variability of V564 Her was discovered by Hoffmeister (1966b). Following Thänert (1974), the variable was classified in the GCVS as an RRAB star with the light elements JD = 2429374.544 + 0.4028257×E. According to the data from ROTSE-I/NSVS, SWASP, and Catalina surveys, this period is wrong. M – m = 0.17 P. J – K = 0.290 (2MASS). In the NSVS and 1SWASP, V564 Her is blended with GSC 3089-01435, so the amplitude of variability is underestimated.
10. The variability of V572 Her was discovered by Hoffmeister (1966a), the variable was classified as an RR Lyrae star with unknown period. We confirm the RR Lyrae nature of this variable (RRAB type) according to data from Catalina Surveys. The variability period is 0.568058 days. M – m = 0.13 P. J – K = 0.297 (2MASS).
11. V607 Her was reported by Hoffmeister (1968) as an Algol-type star without light elements. Following Busch et al. (1974), the variable was classified in the GCVS as an eclipsing variable star (EA/SD type) with the elements JD(min) = 2439538.619 + 3.425200×E. This period is wrong. According to data from 1SWASP, ROTSE-I/NSVS, ASAS, and Catalina surveys, the period is twice shorter (P = 1.712532 days). D = 0.14 P. MinII = 12.m9 (CV). From the 1SWASP data: 12.m70 – 13.m45, MinII = 12.m83 (WASP mag); from the ASAS-3: 12.m8 – 13.m6 (V); from the ROTSE-I/NSVS: 13.m13 – 13.m85, MinII = 13.m30 (R).
12. The variability of V630 Her was discovered by Richter (1969). The variable was classified as an RR Lyrae star (RR) without light elements. Following Thänert (1974), the variable was classified in the GCVS as an RRAB star with the elements JD(max) = 2430103.513 + 0.476151×E. This period is wrong. According to data from Catalina Surveys, P = 0.607739 days. M – m = 0.15 P. J – K = 0.415 (2MASS).
13. The variability of V678 Her was discovered by Hoffmeister (1968) who had found the Algol type and could not determine the light elements. Following Busch et al. (1974), the variable was classified in the GCVS as an EA star with the light elements JD(min) = 2439889.406 + 1.389665×E. According to data from Catalina Surveys, the true period is somewhat longer. D = 0.14 P. MinII = 14.m60 (CV).
14. The variability of V680 Her was discovered by Hoffmeister (1966b). The variable was classified as a possible short-period star without light elements. Following Busch et al. (1974), the variable was classified in the GCVS as an RR Lyrae star (RRAB) with the light elements JD(max) = 2439940.491 + 0.660136×E. This period is wrong. According to data from Catalina Surveys and LINEAR, it is actually a double-mode RR Lyrae star that pulsates in the first-overtone and fundamental modes. The light elements are tabulated below.P1/P0 = 0.7453. J – K = 0.295 (2MASS).
Mode Frequency, c/d Semi-amplitude, Mag Period, days Epoch, JD f1 2.515141 0.146 (CV), 0.146 (LINEARmag) 0.397592 2454800.810 f0 1.874555 0.092 (CV), 0.088 (LINEARmag) 0.533460 2454800.903 f1 + f0 4.38962 0.039 (CV) 0.227810 2454800.616 f1 – f0 0.640517 0.032 (CV) 1.56124 2454800.57
15. The variability of V689 Her was reported by Richter (1969), rapid variations were suspected. Following Busch et al. (1974), the variable was classified in the GCVS as an eclipsing binary (type E), with a possible period of 3.07/N days (mag. range 15.m6 – 16.m0 pg). According to data from Catalina survey, V689 Her is a constant star, its variability is not confirmed.
16. The variability of V696 Her was reported by Richter (1969). The variable was classified as an eclipsing star (E type) without light elements. Following Busch et al. (1974), the variable was classified in the GCVS as an IS: variable. (mag. range 15.m6 – 16.m6 pg). Based on the data from Catalina survey, we do not confirm the star's variability.
17. The variability of V699 Her was discovered by Richter (1969). The variable was classified as a possible rapid variable. Following Busch et al. (1974), the variable was classified in the GCVS as an eclipsing binary (type EW/KE), mag. range 15.m4 – 16.m2 (pg), with the light elements JD(min) = 2439529.600 + 0.614205 x E. According to data from Catalina Surveys, V699 Her is a constant star, its variability is not confirmed.
18. The variability of V703 Her was reported by Richter (1969). The variable was classified as a possible fast variable. Following Busch et al. (1974), the variable was classified in the GCVS as an RR Lyrae star (RR) without light elements, mag. range 15.m3 – 16.m1 (pg). In contradiction with previous studies, data from Catalina Surveys shows V703 Her to be a constant star.
19. The variability of V710 Her was reported by Richter (1969). Following Busch et al. (1974), the variable was classified in the GCVS as a possible RR Lyrae star without light elements, mag. range 16.m6 – 17.m4 (pg). According to data from Catalina Surveys, its variability is not confirmed.
20. The variability of V723 Her was discovered by Kurochkin (1977). Based on his results, the variable was classified in the GCVS as an eclipsing binary (type EA/SD:) with the light elements JD(max) = 2440832.374 + 3.967052: ×E. We confirm the eclipsing nature of this variable (EA type) using data from SWASP and Catalina Surveys but do not confirm the period. D = 0.06 P. MinII = 14.m61 (CV). From the 1SWASP data: 14.m4 – 15.m0 (SWASPmag), MinII = 14.m6 (SWASPmag).
21. The variability of V757 Her was discovered by Kurochkin (1977). The variable was classified in the GCVS as a possible eclipsing binary (type E:) without light elements, mag. range 13.m4 – 14.m2 (pg). Meinunger (1983) did not find any variability, V757 Her was classified as a red constant star with the magnitude 13.m6 (pg). According to ROTSE-I/NSVS and SWASP data, it is a posiible SR star. From the ROTSE-I/NSVS data: 11.m2 – 11.m55 in the R band; from the CSS data: 10.m95 – 11.m64 (CV).
J – K = 0.978 (2MASS), B – V = 2.057 (Tycho2).
22. The variability of V769 Her was discovered by Kurochkin (1977). From his data, the variable was classified as a possible long-period eclipsing binary (type E:), mag. range 13.m8 – 16.m1 (pg). According to ROTSE-I/NSVS and SWASP data, V769 Her is an LB star. From the 1SWASP data: 11.m6 – 11.m95 (1SWASPmag); from the ROTSE-I/NSVS data: 10.m55 – 10.m85 in the R band. J – K = 1.223 (2MASS). Spectral type M3-M4III (FBS-L 1724+470, Gigoyan et al. 2010). NSVS and SWASP data shows the variable blended with GSC 3512-00114, the variability amplitude is underestimated.
23. The variability of V801 Her was discovered by Hoffmeister (1966a), the variable was classified as a slow variable, mag. range 15.m0 – 15.m5 (pg). Following Gessner (1983), the variable was classified in the GCVS as a semiregular variable star (SR type, P = 268 days). According to data from Catalina Surveys, it is actually an RR Lyrae star (RRAB type). M – m = 0.18 P.
J – K = 0.320 (2MASS).
24. The variability of V1070 Her was discovered by Akerlof et al. (2000) based on the ROTSE-I/NSVS data. Diethelm (2001) gives the EA type and the following light elements: HJD = 2451265.8306 + 1.2661×E. We reinvestigated the star using the same ROTSE-I/NSVS data and the data from SWASP and Catalina surveys. We confirm the eclipsing nature of this variable but with a twice longer orbital period. D = 0.16 P. MinII = 12.m1 (WASPmag). From the ROTSE-I/NSVS data: 12.m0 – 13.m6,
MinII = 12.m1 in the R band; from the CSS data: 11.m75 – 13.m1 (CV).Remarks:
We have looked through the GCVS list of variable stars in the constellation Hercules (Samus et al. 2007 – 2012), analyzed all available observations of these stars from the Catalina Surveys (Drake et al. 2009), SuperWASP (Butters et al. 2010), ROTSE-I/NSVS (Woźniak et al. 2004), ASAS-3 (Pojmanski 2002), and LINEAR (Sesar et al. 2011) online public archives and found twenty four stars for which the information contained in the GCVS and VSX databases (classification, light elements) can be verified or changed.
The SuperWASP observations are available as FITS tables which were converted into ASCII tables using the OMC2ASCII program as described by Sokolovsky (2007).
Acknowledgements: The study was supported, in part, by the Russian Foundation for Basic Research through grants No. 11-02-00495 and 13-02-00664. Thanks are due to Dr. K.V. Sokolovsky for his advice concerning data retrieving. The authors wish to thank Dr. V.P. Goranskij for providing his software.References:
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