Peremennye Zvezdy

Article in PDF
"Peremennye Zvezdy",
Prilozhenie
,
vol. 23, N 2 (2023)

New Light Elements for Seventeen Stars of Different Variability Types

E. V. Kazarovets
Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

ISSN 2221–0474 DOI: 10.24412/2221-0474-2023-2-1

Received:   22.05.2023;   accepted:   6.07.2023
(E-mail for contact: helene@inasan.ru)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1NSV 049592MASS J10442678-601129610 44 26.78 -60 11 29.7EA13.5613.94V0.6944352458148.704min Comm. 1lc_NSV04959.pngch_NSV04959.pngdat1.txt
2NSV 05993USNO-A2.0 0525-1551006512 51 31.01 -34 23 50.2RRC15.1415.53V0.3836712457178.602max Comm. 2lc_NSV05993.pngch_NSV05993.pngdat2.txt
3 USNO-B1.0 0393-070070917 51 44.87 -50 38 25.4EA14.1414.32g0.8000482459454.488min Comm. 3lc_175144-5038.pngch_175144-5038.pngdat3.txt
4 USNO-B1.0 0567-075749318 02 40.31 -33 14 14.8M15.24<17.5V2792457851max Comm. 4lc_180240-3314.pngch_180240-3314.pngdat4.txt
5 GSC 6851-0223018 11 33.20 -27 43 39.8SR13.3315.8 :g178.82459502.3max Comm. 5lc_181133-2743.pngch_181133-2743.pngdat5.txt
6 USNO-A2.0 0525-3319084518 12 33.09 -31 57 30.7M14.46<16.9V2992458022max Comm. 6lc_181233-3157.pngch_181233-3157.pngdat6.txt
7 GSC 6861-02553 N18 33 13.12 -24 57 50.1M12.3516.12zr203.02459511.5max Comm. 7lc_183313-2457.pngch_183313-2457.pngdat7.txt
8NSV 13623BD-20 616721 16 09.37 -20 11 33.9ELL11.2211.25g1.347842459423.669min Comm. 8lc_NSV13623.pngch_NSV13623.pngdat8.txt
9 USNO-A2.0 1500-0856969321 56 03.24 +61 05 51.9EA15.6315.93zg25.5842459047.781min Comm. 9lc_215603_6105.pngch_215603_6105.pngdat9.txt
10 USNO-A2.0 1500-0863249121 59 12.23 +60 46 35.6EA14.3514.78zr10.70972458761.708min Comm. 10lc_215912_6046.pngch_215912_6046.pngdat10.txt
11 USNO-B1.0 1497-033199422 00 44.42 +59 45 00.5DCEP15.2515.90zr15.63362458593.924max Comm. 11lc_220044_5945.pngch_220044_5945.pngdat11.txt
12 USNO-A2.0 1425-1398463522 44 41.22 +54 03 54.0RCB:14.4215.77zr  other Comm. 12lc_224441_5403.pngch_224441_5403.pngdat12.txt
13 USNO-A2.0 1425-1399969122 45 11.03 +54 55 51.4EA14.0414.15zr3.408852458759.782min Comm. 13lc_224511_5455.pngch_224511_5455.pngdat13.txt
14 USNO-A2.0 1425-1403684122 46 25.07 +54 16 55.7EA14.3414.44g1.050382459443.837min Comm. 14lc_224625_5416.pngch_224625_5416.pngdat14.txt
15 USNO-A2.0 1425-1405443122 47 00.98 +52 52 33.9EA/RS15.1215.52zr7.39462458442.74min Comm. 15lc_224701_5252.pngch_224701_5252.pngdat15.txt
16 USNO-A2.0 1425-1415844322 50 31.21 +53 51 34.2EA13.7214.12V9.22542458762.825min Comm. 16lc_225031_5351.pngch_225031_5351.pngdat16.txt
17 USNO-A2.0 1425-1420022222 51 58.54 +53 18 50.6EA15.5215.77zg2.181562458819.616min Comm. 17lc_225158_5318.pngch_225158_5318.pngdat17.txt

Comments:


1. Min II = 13.69 V, D = 0.20 P. The star was included in ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with a type EA and P = 1.3888681 d.

2. M – m = 0.35 P. The star was included in ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with a type CWB and P = 1.1509774 d.

3. Min II = 14.24 g, D = 0.12 P. Variability was discovered by the author using the ASAS-SN photometric data.

4. = ASASSN-V J180240.32-331414.9 (see Iwanek et al. 2022). Variability of this star was independently discovered by the author using the STScI plates archive.

5. Variability of this star was discovered by the author using the STScI plates archive.

6. Variability of this star was discovered by the author using the STScI plates archive. The star was included in ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with the type YSO and no period. The ASAS-SN photometry in V- and g-bands in common was used for period determination. Magnitudes in g were adjusted by –1 mag.

7. N-comp. of 3" pair. Variability of this star was discovered by the author using the STScI plates archive. The ASAS-SN photometry in V- and g-bands, and ZTF photometry in zr-band in common were used for period determination. Magnitudes in g were adjusted by –1 mag.

8. Min II = 11.23 g. The star was suspected by Borrelly (1885) who did not publish a finding chart. Recovered by the author using the ASAS-SN photometric data.

9. Min II = 15.89 zg, D = 0.02 P. Min II – Min I = 0.785 P. The variability was discovered by Lapukhin et al. (2018a) who published an incorrect P = 4.16: d.

10. Min II = 14.55 zr, D = 0.02 P. Min II – Min I = 0.68 P. The variability was discovered by Lapukhin et al. (2018b) who published an incorrect P = 1.7708: d.

11. M – m = 0.40 P. Blazhko effect. The variability was discovered by Lapukhin et al. (2018a) who gave type BY and erroneous P = 16.24 d.

12. Pulsation cycle P ~ 73 d. The variability was discovered by Lapukhin et al. (2020) with a type LB. The star was included in the ZTF Catalog of Variable Stars (Chen et al. 2020) with a type SR and P = 70.4 d.

13. Min II = 14.06 zr, D = 0.04 P. The variability of 2MASS J22451103+5455516 was discovered by Lapukhin et al. (2020) with incorrect P = 1.4045: d.

14. Min II = 14.42 g, D = 0.08 P. The variability of 2MASS J22462507+5416558 was discovered by Lapukhin et al. (2020) with incorrect P = 0.68802 d and a type EW. There is a faint companion at 2".2 N. It is not excluded that the companion is the actual variable.

15. Min II = 15.22 zr, D = 0.08 P. Distortion wave P = 7.36 d. The variability of 2MASS J22470097+5252338 was discovered by Lapukhin et al. (2020) with incorrect P = 2.3786: d and a type EA.

16. Min II = 13.81 V, D = 0.03 P. Min II - Min I = 0.460. The variability of 2MASS J22503120+5351341 was discovered by Lapukhin et al. (2021) with incorrect P = 1.8013: d.

17. Min II = 15.62 zg, D = 0.05 P. The variability of 2MASS J22515854+5318505 was discovered by Lapukhin et al. (2021) with incorrect P = 0.727191 d.

Remarks:
While working on compiling of the next Name-List for Version 5.1 of the General Catalogue of Variable Stars (GSVS, Samus et al. 2017), I determined types, light elements and improved coordinates for 4 new variable stars, 3 more stars from the NSV catalogue (Kazarovets et al. 2022) and 10 new variables, discovered and published by other authors to transfer them to the GCVS. The study of the variables was made using the publicly available electronic archive of CCD observations of the Sky Patrol of the All-Sky Automated Survey for Supernovae (ASAS-SN) project (Shappee et al. 2014, Kochanek et al. 2017) and the Zwicky Transient Facility (ZTF) photometric data (Masci et al. 2019). For each star, I present archive observations. Information on the filter can be found in corresponding files.

To find periods I applied the WinEfk software provided by Dr. V.P. Goranskij and the on-line lightcurve analysis tool created by Dr. K.V. Sokolovsky.

References:
Borrelly, M.A., 1885, Bulletin astronomique, 2, 62
Chen, X., Wang, S., Deng, L., et al., 2020, Astrophys. J. Suppl., 249, 18
Iwanek, P., Soszyński, I., Kozłowski, S., et al., 2022, Astrophys. J. Suppl. Ser., 260, 46
Jayasinghe, T., Stanek, K.Z., Kochanek, C.S., et al., 2018, Mon. Not. Royal Astron. Soc., 486, No. 2, 1907
Kochanek, C.S., Shappee, B.J., Stanek, K.Z., et al., 2017, Publ. Astron. Soc. Pacific, 129, No. 980, 104502
Kazarovets, E.V., Samus, N.N., and Durlevich, O.V., 2022, Astron. Rep., 66, No. 7, 555
Lapukhin, E.G., Veselkov, S.A., and Zubareva, A.M., 2018a, Perem. Zvezdy Prilozh. (Var. Stars Suppl.), 18, No. 1
Lapukhin, E.G., Veselkov, S.A., and Zubareva, A.M., 2018b, Perem. Zvezdy Prilozh. (Var. Stars Suppl.), 18, No. 2
Lapukhin, E.G., Zubareva, A.M., Kryukova, E., and Khamrakulov, F., 2020, Perem. Zvezdy Prilozh. (Var. Stars Suppl.), 20, No. 2
Lapukhin, E.G., Zubareva, A.M., Kryukova, E., and Khamrakulov, F., 2021, Perem. Zvezdy Prilozh. (Var. Stars Suppl.), 21, No. 3
Masci, F.J., Laher, R.R., Rusholme, B., et al., 2019, Publ. Astron. Soc. Pacific, 131, No. 995, 018003
Samus, N.N., Kazarovets, E.V., Durlevich, O.V., Kireeva, N.N., Pastukhova, E.N., 2017, Astron. Rep. 61, No. 1, 80
Shappee, B.J., Prieto, J.L., Grupe, D., et al., 2014, Astrophys. J., 788, 48



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