Peremennye Zvezdy

"Peremennye Zvezdy",
Prilozhenie
,
vol. 13, N 15 (2013)

New Data for Known Variables in Hercules

S. V. Antipin#1,2, A. V. Khruslov#2
#1. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow, Russia;
#2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

Received:   25.05.2013;   accepted:   29.10.2013
(E-mail for contact: antipin@sai.msu.ru, khruslov@bk.ru)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1HH HerGSC 2582-0113116 38 40.48, +31 38 44.2CST15.20 CV  other Comm. 11.PNGchart1.PNGCSS_data_1.txt
2V368 HerUSNO-A2.0 1050-0842491417 10 31.09, +22 23 08.4RRAB15.0315.50CV1.1914752454703.677max Comm. 22.PNGchart2.PNGCSS_data_2.txt
3V413 HerGSC 2083-0160517 31 35.62, +26 42 04.0RRAB14.9415.64CV1.055232454800.740max Comm. 33.PNGchart3.PNGCSS_data_3.txt
4V426 HerGSC 2076-0004617 35 29.05, +23 01 27.7RRC14.7015.10CV0.3263662454800.600max Comm. 44.PNGchart4.PNGCSS_data_4.txt
5V470 HerGSC 2061-0103517 14 14.90, +24 02 20.5EA15.3515.94CV2.500292454704.650min Comm. 55.PNGchart5.PNGCSS_data_5.txt
6V517 HerUSNO-A2.0 1050-0901714417 41 34.94, +19 24 56.4RRAB15.6816.80CV0.4803962454700.873max Comm. 66.PNGchart6.PNGCSS_MLS_data_6.txt
7V541 HerUSNO-A2.0 1050-0792095116 24 05.04, +18 48 24.4RRAB14.2415.53CV(see Comments)(see Comments)max Comm. 77.PNGchart7.PNGCSS_data_7.txt
8V561 HerUSNO-A2.0 1125-0866575817 51 30.05, +28 22 12.6RRAB15.6316.43CV0.5799762454800.770max Comm. 88.PNGchart8.PNGCSS_data_8.txt
9V564 HerUSNO-A2.0 1275-0968088017 58 17.42, +38 21 18.4RRAB14.5115.32CV0.6744762454600.835max Comm. 99.PNGchart9.PNGCSS_data_9.txt 1SWASP_data_9.txt NSVS 5365334 NSVS 8065821 NSVS 8083188
10V572 HerUSNO-A2.0 1125-0910064618 11 38.37, +25 54 39.1RRAB14.4615.54CV0.5680582454500.949max Comm. 1010.PNGchart10.PNGCSS_data_10.txt
11V607 HerGSC 2053-0004616 40 54.50, +26 22 10.1EA12.713.49CV1.7125322454000.91min Comm. 1111.PNGchart11.PNGCSS_data_11.txt 1SWASP_data_11.txt NSVS 7894581 ASAS 164054+2622.2
12V630 HerUSNO-A2.0 1200-0890254418 05 10.18, +31 56 17.3RRAB16.0516.89CV0.6077392454700.575max Comm. 1212.PNGchart12.PNGCSS_data_12.txt
13V678 HerGSC 2035-0055316 08 16.66, +24 42 13.7EA14.4615.55CV1.4537442454640.897min Comm. 1313.PNGchart13.PNGCSS_data_13.txt
14V680 HerUSNO-A2.0 1050-0780639216 10 22.75, +21 48 26.6RR(B)15.3115.98CV(see Comments)(see Comments)max Comm. 1414.PNGchart14.PNGCSS_data_14.txt LINEAR_data_14.txt
15V689 HerGSC 1505-0118716 17 13.33, +16 38 54.0CST14.95 CV  other Comm. 1515.PNGchart15.PNGCSS_data_15.txt
16V696 HerGSC 1510-0016916 28 08.71, +18 29 34.9CST14.2 CV  other Comm. 1616.PNGchart16.PNGCSS_data_16.txt
17V699 HerGSC 1510-0119516 30 33.07, +17 00 47.0CST14.85 CV  other Comm. 1717.PNGchart17.PNGCSS_data_17.txt
18V703 HerUSNO-A2.0 1050-0800156216 33 26.50, +21 29 16.2CST16.4 CV  other Comm. 1818.PNGchart18.PNGCSS_data_18.txt
19V710 HerUSNO-A2.0 1050-0811625816 45 24.86, +18 27 36.1CST16.5 CV  other Comm. 1919.PNGchart19.PNGCSS_data_19.txt
20V723 HerGSC 3077-0089517 11 11.84, +40 43 52.8EA14.3515.00CV8.06342454273.48min Comm. 2020.PNGchart20.PNGCSS_data_20.txt 1SWASP_data_20.txt
21V757 HerGSC 3501-0168917 13 22.83, +45 38 00.3SR:11.712.1WASP48.42454246other Comm. 2121.PNGchart21.PNG1SWASP_data_21.txt NSVS 5266726 NSVS 5304463 NSVS 5332739
22V769 HerGSC 3512-0022517 25 57.38, +47 02 51.1LB13.816.1p  otherM3-M4IIIComm. 2222.PNGchart22.PNG1SWASP_data_22.txt NSVS 5312353
23V801 HerGSC 0990-0068117 20 23.89, +13 32 40.0RRAB14.4415.19CV0.4983712454600.670max Comm. 2323.PNGchart23.PNGCSS_MLS_data_23.txt
24V1070 HerGSC 2619-0083317 49 53.05, +37 08 39.8EA11.9513.5WASP2.532102453182.648min Comm. 2424.PNGchart24.PNGCSS_data_24.txt 1SWASP_data_24.txt NSVS 8057960 NSVS 5358358 NSVS 8075737

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:
ModeFrequency, 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.
ModeFrequency, 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
P1/P0 = 0.7453. J – K = 0.295 (2MASS).

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:
Ahnert, P., van Schewick, H., Hoffmeister, C., 1941, Kleine Veröff. Berlin-Babelsberg, Nr. 24
Akerlof, C., Amrose, S., Balsano, R., et al., 2000, Astron. J., 119, 1901
Busch, H., Häussler, K., Thänert, C., 1974, Veröff. Sternwarte Sonn., 8, 177
Butters, O.W., West, R.G., Anderson, D.R., et al., 2010, Astron. and Astrophys., 520, L10
Diethelm, R., 2001, Inform. Bull. Var. Stars, No. 5060
Drake, A.J., Djorgovski, S.G., Mahabal, A., et al., 2009, Astrophys. J., 696, 870
Drake, A.J., Catelan, M., Djorgovski, S.G., et al, 2013, Astrophys. J., 763, 20
Gessner, H., 1983, Mitt. Veränderliche Sterne, 9, 116
Gigoyan, K.S., Sinamyan, P.K., Engels, D., Mickaelian, A.M., 2010, Astrophysics, 53, 123
Hoffmeister, C., 1936, Astron. Nachr., 259, 37
Hoffmeister, C., 1949, Astronomishe Abhandlungen, Ergänzunghefte zu den Astron. Nachr., 12, N. 1
Hoffmeister, C., 1959, Astron. Nachr., 284, 275
Hoffmeister, C., 1960, Veröff. Sternwarte Sonn., 4, 315
Hoffmeister, C., 1966a, Astron. Nachr., 289, 1
Hoffmeister, C., 1966b, Astron. Nachr., 289, 139
Hoffmeister, C., 1968, Astron. Nachr., 290, 277
Kinemuchi, K., Smith, H.A., Woźniak, P.R., McKay, T.A., 2006, Astron. J., 132, 1202
Kurochkin, N.E., 1977, Perem. Zvezdy Prilozh., 3, 201
Meinunger, L., 1983, Mitt. Veränderliche Sterne, 10, 1
Pojmanski, G., 2002, Acta Astronomica, 52, 397
Ponomareva, G.A., 1969, Astron. Tsirk., No. 532, 1
Richter, G., 1969, Mitt. Veränderliche Sterne, 5, 68
Samus, N.N., Durlevich, O.V., Kazarovets, E.V., et al., 2007 – 2012, General Catalogue of Variable Stars, Centre de Données Astronomiques de Strasbourg, B/gcvs
Sesar, B., Stuart, J.S., Ivezić, Ž., et al., 2011, Astron. J., 142, 190
Sokolovsky, K.V., 2007, Perem. Zvezdy Prilozh., 7, No. 30
Thänert, C., 1974, Veröff. Sternvarte Sonn., 8, 215
Woźniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004, Astron. J., 127, 2436



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