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.
| 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 |
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:
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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
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Butters, O.W., West, R.G., Anderson, D.R., et al., 2010, Astron. and Astrophys.,
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Diethelm, R., 2001, Inform. Bull. Var. Stars, No. 5060
Drake, A.J., Djorgovski, S.G., Mahabal, A., et al., 2009, Astrophys. J., 696,
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Drake, A.J., Catelan, M., Djorgovski, S.G., et al, 2013, Astrophys. J., 763, 20
Gessner, H., 1983, Mitt. Veränderliche Sterne, 9, 116
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