Peremennye Zvezdy

"Peremennye Zvezdy",
Prilozhenie
,
vol. 16, N 3 (2016)

40 Red Variable Stars: Variability Types and Light Elements

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

Received:   28.12.2015;   accepted:   29.04.2016
(E-mail for contact: Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 2MASS 17433740-404316517 43 37.40, -40 43 16.6M13.0<16.5V2122454950max  1lc.jpg1ch.jpgASAS 174337-4043.3
2 2MASS 18063887-413702518 06 38.88, -41 37 02.5M12.5<14.8V1912453844max  2lc.jpg2ch.jpgASAS 180639-4137.0
3NSV 10232S 986418 07 31.53, +04 15 32.4SR12.514.2V5402453900max Comm. 310232lc.jpg10232ch.jpgASAS 180731+0415.5
4NSV 10237HV 722018 08 34.27, -36 40 57.8SR12.313.2V8602454500max Comm. 410237lc.jpg10237ch.jpgASAS 180834-3641.0
5 2MASS 18092874-340740618 09 28.75, -34 07 40.6M12.4<15.0V2272454371max  5lc.jpg5ch.jpgASAS 180929-3407.7
6NSV 10285HD 16610518 09 43.05, -15 16 56.9LB7.68.8V  otherM1Iab 10285lc.jpg10285ch.jpgASAS 180943-1517.0
7NSV 10348HV 978818 13 03.02, -49 40 31.7SR12.1513.6V2182454917max  10348lc.jpg10348ch.jpgASAS 181303-4940.5
8NSV 10387S 987018 13 15.14, +03 46 02.6SR10.811.5V4202454760max  10387lc.jpg10387ch.jpgASAS 181315+0346.1
9NSV 10402GSC 6843-0045518 14 36.04, -23 58 01.9SR11.912.7V5902454572maxM5: 10402lc.jpg10402ch.jpgASAS 181436-2358.0
10 GSC 9055-0248618 15 17.99, -61 15 38.9SR12.313.5V57.72454763max  10lc.jpg10ch.jpgASAS 181518-6115.6
11NSV 10643GSC 6852-0509118 20 33.13, -28 02 54.0SR12.514.0V1202454994max  10643lc.jpg10643ch.jpgASAS 182033-2802.9
12NSV 10667 18 21 28.14, -23 53 33.6SR:13.0<15V1922455013maxM7Comm. 1210667lc.jpg10667ch.jpgASAS 182128-2353.6
13NSV 10700 18 22 36.03, -24 30 48.7M13.1<15.4V2872454306max Comm. 1310700lc.jpg10700ch.jpgASAS 182236-2430.8
14NSV 10711GSC 6844-0156518 23 09.55, -24 21 55.8SR12.113.1V96.42455040maxM2 10711lc.jpg10711ch.jpgASAS 182310-2421.9
15NSV 10740S 989118 23 58.65, +07 26 59.2SR11.111.9V4322454725max Comm. 1510740lc.jpg10740ch.jpgASAS 182359+0727.0
16NSV 10728HV 989018 25 11.64, -58 09 31.6SR10.612.5V1562454769max Comm. 1610728lc.jpg10728ch.jpgASAS 182512-5809.5
17NSV 10830HV 944018 28 32.97, -45 59 27.7SR10.312.8V1842455005max Comm. 1710830lc.jpg10830ch.jpgASAS 182833-4559.5
18NSV 10838S 504518 29 03.33, -52 54 05.3SR9.510.6V4692455100maxM2IIIComm. 1810838lc.jpg10838ch.jpgASAS 182903-5254.1
19NSV 10974HV 945918 32 05.18, -17 02 01.8M12.9<15.5V2392454590max  10974lc.jpg10974ch.jpgASAS 183205-1702.0
20NSV 10949HV 945118 32 20.27, -44 50 53.2M13.7<17.2V493:2454585max Comm. 2010949lc.jpg10949ch.jpgASAS 183220-4450.9
21NSV 11027HV 946518 33 14.00, -29 54 58.7M12.9<15.6V2902454667max  11027lc.jpg11027ch.jpgASAS 183314-2955.0
22NSV 11011 18 33 32.00, -22 47 36.5SR13.013.9:V3342454250max  11011lc.jpg11011ch.jpgASAS 183332-2247.6
23NSV 10990HV 945418 33 32.62, -49 12 43.0SR12.614.0V4652454680max Comm. 2310990lc.jpg10990ch.jpgASAS 183332-4912.7
24NSV 11026HV 946418 34 08.12, -26 44 59.2M12.6<16.6V2732454906max Comm. 2411026lc.jpg11026ch.jpgASAS 183408-2645.0
25NSV 11019S 739418 34 23.67, -44 27 22.2M13.0<16.2V3032454921max  11019lc.jpg11019ch.jpgASAS 183424-4427.4
26NSV 11063HV 947718 35 57.03, -29 14 31.9M12.0<14.7V196.52455093max  11063lc.jpg11063ch.jpgASAS 183557-2914.5
27NSV 11030S 711818 36 05.21, -63 33 06.3M11.7<14.9V2692454607max  11030lc.jpg11030ch.jpgASAS 183605-6333.1
28NSV 11174GSC 6280-0122318 40 16.15, -15 13 43.6SRA12.413.9V3952455078maxM7Comm. 2811174lc.jpg11174ch.jpgASAS 184016-1513.7
29NSV 11186HV 949918 40 48.98, -28 37 39.9M12.0<15.0V4332455049max Comm. 2911186lc.jpg11186ch.jpgASAS 184048-2837.8
30NSV 11226BV 170418 42 37.21, -18 26 31.0M12.4<16.2V2052454942max  11226lc.jpg11226ch.jpgASAS 184237-1826.5
31NSV 11232HV 950618 43 24.58, -46 19 06.5M12.3<15.6V2032455014max Comm. 3111232lc.jpg11232ch.jpgASAS 184325-4619.1
32NSV 11242BV 125418 45 08.27, -65 27 31.3SR10.210.85V3382454780max Comm. 3211242lc.jpg11242ch.jpgASAS 184508-6527.5
33NSV 11285HV 951818 45 08.44, -25 16 21.8M13.0<16.6V2802454266max  11285lc.jpg11285ch.jpgASAS 184508-2516.4
34NSV 11277Innes 5918 45 17.33, -33 32 15.1M12.6<14.2V3342454967max  11277lc.jpg11277ch.jpgASAS 184517-3332.3
35NSV 11371S 963918 48 18.45, +40 17 55.1SR11.8512.95*123.82455105max Comm. 3511371lc.jpg11371ch.jpg11371dat.txt
36NSV 11392 18 49 57.30, +20 32 12.9M12.5<15.5V3162454208maxMeComm. 3611392lc.jpg11392ch.jpgASAS 184957+2032.2
37NSV 11403224.193018 50 14.14, +15 20 38.1M13.0<15.4V3022454691max  11403lc.jpg11403ch.jpgASAS 185014+1520.6
38NSV 11394HV 954318 50 28.65, -16 36 56.0M12.0<14.0V269.52454973max  11394lc.jpg11394ch.jpgASAS 185029-1636.9
39NSV 11415BV 170918 51 20.86, -14 26 06.8SR13.114.5:V1442454663max  11415lc.jpg11415ch.jpgASAS 185121-1426.1
40NSV 11398BV 81318 51 21.93, -43 05 55.4SR10.911.9V3282454880max Comm. 4011398lc.jpg11398ch.jpgASAS 185122-4306.0

Comments:


3. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 192d.7.

4. Superposed variations of P = 95d.5. HV 7220 was found, upon our request, by the late Dr. M.Hazen in Harvard Observatory's logbooks. No finding chart was available for this variable before.

12. The ASAS-3 range is for the combined brightness of the variable star and its neighbor. Variable is the SE component of 4" pair. Mira type for this variable is not excluded.

13. One well-defined maximum (JD = 2431620) observed by Hoffleit (1964) was used to improve our elements.

15. Superposed variations of P = 48d.0. Variability was discovered in the ASAS-3 survey; the starenters their variable-star catalog as a MISC-type star with a wrong period of 168d.5.

16. HV 9890 was found, upon our request, by the late Dr. M.Hazen in Harvard Observatory's logbooks. No finding chart was available for this variable before.

17. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 122d.2.

18. Superposed variations of P = 52d.3. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 63d.4.

20. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

23. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 180d.

24. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

28. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 183d.7.

29. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 142d.1.

31. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

32. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 41d.6.

35. We study the variability of NSV 11371 using the Northern Sky Variability Survey (NSVS) unfiltered data (Woźniak et al. 2004a), but epoch of maximum brightness used is from the online publicly available Catalina Sky Survey data (2013) for CSS J184818.4+401757.

36. This star, NSVS J1849573+203211, was studied by Woźniak et al. (2004b), they gave the Mira type and a wrong period of 282d.

40. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 175d.3.

Remarks:
As a part of our work on improvement of coordinates of variable stars in the NSV catalog (Samus et al. 2007–2015), we derived light elements and types for 40 red stars. We recovered the following variables suspected by W.J. Luyten: HV 9459, HV 9464, HV 9477, HV 9499, and HV 9518 (Luyten 1937); HV 9465 (Luyten 1935); HV 9454 and HV 9506 (Luyten 1936); and also the stars Innes 59 suspected by Innes (1914) and BV 813 suspected by Strohmeier et al. (1966). We measured minimal brightness for many Mira variables in Digitized Sky Survey images (R-band). We studied the variables using the publicly available electronic archives of CCD observations of the ASAS-3 project (Pojmanski 2002), and images of the STScI and US Naval Observatory Image and Catalog Archive. We found and investigated four new long-period variable stars: 2MASS 17433740-4043165, 2MASS 18063887-4137025, 2MASS 18092874-3407406, and GSC 9055-02486.

Acknowledgments: Our studies are supported by a grant from the Program "Transition and explosive processes in the Universe" of the Presidium of Russian Academy of Sciences.

References:
Hoffleit, D., 1964, Astron. J., 69, 301
Innes, R., 1914, Circ. Union Obs., No. 20
Luyten, W.J., 1935, Astron. Nachr., 256, 325
Luyten, W.J., 1936, Astron. Nachr., 258, 121
Luyten, W.J., 1937, Astron. Nachr., 261, 451
Pojmanski, G., 2002, Acta Astron., 52, 397
Samus, N.N., Durlevich, O.V., Goranskij, V.P., Kazarovets, E V., Kireeva, N.N., Pastukhova, General Catalogue of Variable Stars, Centre de Données Astronomiques de Strasbourg, B/gcvs
Strohmeier, W., Fischer, H., Ott, H., 1966, Inform. Bull. Var. Stars, No. 140
Woźniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004a, Astron. J., 127, 2436
Woźniak, P.R., Williams, S.J., Vestrand, W.T., Gupta, V., 2004b, Astron. J., 128, 2965



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