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Дата изменения: Mon Jan 29 11:46:08 1973 Дата индексирования: Fri Feb 28 14:24:42 2014 Кодировка: Поисковые слова: m 5 |
Peremennye Zvezdy (Variable Stars) 33, No. 4, 2013 Received 04 June; accepted 25 June.
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We present our discovery a new variable star USNO-A2.0 1350-17086180 from observations at the Astrotel-Caucasus Observatory. The object shows Algol-type eclipses and, simultaneously, low-amplitude, short-period pulsations. |
Night | JD | No.of | Night | JD | No. of | Night | JD | No. of |
No. | observations | No. | observations | No. | observations | |||
1 | 2455828 | 11 | 16 | 2455925 | 40 | 31 | 2456185 | 48 |
2 | 2455833 | 50 | 17 | 2455926 | 20 | 32 | 2456186 | 48 |
3 | 2455842 | 50 | 18 | 2455930 | 38 | 33 | 2456188 | 28 |
4 | 2455843 | 60 | 19 | 2455956 | 28 | 34 | 2456189 | 52 |
5 | 2455873 | 72 | 20 | 2456109 | 7 | 35 | 2456190 | 51 |
6 | 2455879 | 75 | 21 | 2456115 | 19 | 36 | 2456195 | 44 |
7 | 2455880 | 95 | 22 | 2456116 | 5 | 37 | 2456196 | 45 |
8 | 2455881 | 72 | 23 | 2456153 | 21 | 38 | 2456197 | 2 |
9 | 2455883 | 85 | 24 | 2456173 | 2 | 39 | 2456200 | 44 |
10 | 2455884 | 55 | 25 | 2456174 | 40 | 40 | 2456201 | 48 |
11 | 2455888 | 29 | 26 | 2456175 | 42 | 41 | 2456202 | 52 |
12 | 2455895 | 35 | 27 | 2456177 | 40 | 42 | 2456216 | 95 |
13 | 2455900 | 73 | 28 | 2456182 | 53 | 43 | 2456217 | 72 |
14 | 2455901 | 75 | 29 | 2456183 | 45 | 44 | 2456218 | 70 |
15 | 2455902 | 12 | 30 | 2456184 | 44 | 45 | 2456219 | 24 |
For basic reductions for dark current, flat fields, bias and for
removing cosmic rays hits, we used IRAF routines. For photometry
of the new variable star, we applied VaST software by Sokolovsky
and Lebedev (2005). The comparison star was USNO-A2.0
1350-17114431 = USNO-B1.0 1368-0511417 (
,
, J2000,
2MASS;
,
, USNO-B1.0).
Unfiltered magnitudes were calibrated using the comparison star,
assuming
.
All times in this paper are expressed in terrestrial time in accordance with IAU recommendations (resolution B1 XXIII IAU GA).
No. | HJD![]() |
![]() |
1 | 2455881.2869 | 0.0006 |
2 | 2456187.4703 | 0.0004 |
3 | 2456219.3262 | 0.0004 |
The light elements of the primary eclipses are:
Using the prewhitening procedure of the Peranso software, we found
the pulsation period of the Scuti component to be
. The variability amplitude is
, rather
typical of
Scuti stars. During our observations, we
detected 101 maxima of the pulsation light curve, collected in
Table 3.
No. | HJD![]() |
![]() |
![]() |
![]() |
No. | HJD![]() |
![]() |
![]() |
![]() |
1 | 2455842.374 | 0.001 | 0 | 0.000 | 52 | 2456175.426 | 0.003 | 5533 | 0.004 |
2 | 2455842.438 | 0.002 | 1 | 0.004 | 53 | 2456175.484 | 0.001 | 5534 | 0.002 |
3 | 2455842.499 | 0.002 | 2 | 0.005 | 54 | 2456177.412 | 0.002 | 5566 | 0.004 |
4 | 2455843.400 | 0.002 | 17 | 0.003 | 55 | 2456177.472 | 0.002 | 5567 | 0.004 |
5 | 2455843.464 | 0.003 | 18 | 0.007 | 56 | 2456182.345 | 0.005 | 5648 | 0.001 |
6 | 2455843.519 | 0.003 | 19 | 0.001 | 57 | 2456182.404 | 0.003 | 5649 | 0.000 |
7 | 2455873.193 | 0.003 | 512 | 0.000 | 58 | 2456182.468 | 0.003 | 5650 | 0.004 |
8 | 2455873.252 | 0.002 | 513 | -0.001 | 59 | 2456183.427 | 0.002 | 5666 | -0.001 |
9 | 2455873.314 | 0.002 | 514 | 0.001 | 60 | 2456183.489 | 0.002 | 5667 | 0.001 |
10 | 2455873.368 | 0.004 | 515 | -0.005 | 61 | 2456184.393 | 0.004 | 5682 | 0.002 |
11 | 2455873.435 | 0.003 | 516 | 0.001 | 62 | 2456184.456 | 0.003 | 5683 | 0.005 |
12 | 2455879.277 | 0.002 | 613 | 0.005 | 63 | 2456185.416 | 0.002 | 5699 | 0.002 |
13 | 2455879.336 | 0.002 | 614 | 0.003 | 64 | 2456185.478 | 0.002 | 5700 | 0.004 |
14 | 2455879.400 | 0.002 | 615 | 0.007 | 65 | 2456186.384 | 0.002 | 5715 | 0.007 |
15 | 2455879.457 | 0.003 | 616 | 0.004 | 66 | 2456186.445 | 0.003 | 5716 | 0.008 |
16 | 2455880.171 | 0.003 | 628 | -0.004 | 67 | 2456186.502 | 0.002 | 5717 | 0.005 |
17 | 2455880.237 | 0.002 | 629 | 0.002 | 68 | 2456188.483 | 0.002 | 5750 | -0.001 |
18 | 2455880.295 | 0.002 | 630 | -0.001 | 69 | 2456188.545 | 0.002 | 5751 | 0.001 |
19 | 2455880.357 | 0.002 | 631 | 0.001 | 70 | 2456189.384 | 0.002 | 5765 | -0.003 |
20 | 2455880.418 | 0.003 | 632 | 0.002 | 71 | 2456189.451 | 0.002 | 5766 | 0.004 |
21 | 2455880.477 | 0.003 | 633 | 0.001 | 72 | 2456189.508 | 0.002 | 5767 | 0.001 |
22 | 2455881.377 | 0.002 | 648 | -0.002 | 73 | 2456190.415 | 0.004 | 5782 | 0.005 |
23 | 2455881.442 | 0.003 | 649 | 0.003 | 74 | 2456190.472 | 0.005 | 5783 | 0.002 |
24 | 2455883.187 | 0.002 | 678 | 0.002 | 75 | 2456190.539 | 0.003 | 5784 | 0.009 |
25 | 2455883.250 | 0.002 | 679 | 0.005 | 76 | 2456195.406 | 0.002 | 5865 | 0.000 |
26 | 2455883.308 | 0.002 | 680 | 0.003 | 77 | 2456195.464 | 0.003 | 5866 | -0.002 |
27 | 2455883.368 | 0.001 | 681 | 0.003 | 78 | 2456196.429 | 0.002 | 5882 | 0.000 |
28 | 2455883.435 | 0.002 | 682 | 0.009 | 79 | 2456196.488 | 0.002 | 5883 | -0.001 |
29 | 2455884.274 | 0.002 | 696 | 0.006 | 80 | 2456200.412 | 0.002 | 5948 | 0.010 |
30 | 2455884.336 | 0.002 | 697 | 0.007 | 81 | 2456200.464 | 0.004 | 5949 | 0.002 |
31 | 2455884.389 | 0.004 | 698 | 0.000 | 82 | 2456200.524 | 0.003 | 5950 | 0.002 |
32 | 2455884.459 | 0.002 | 699 | 0.010 | 83 | 2456201.427 | 0.002 | 5965 | 0.002 |
33 | 2455888.242 | 0.002 | 762 | 0.001 | 84 | 2456201.549 | 0.001 | 5967 | 0.003 |
34 | 2455895.224 | 0.003 | 878 | 0.001 | 85 | 2456202.391 | 0.003 | 5981 | 0.003 |
35 | 2455895.284 | 0.002 | 879 | 0.000 | 86 | 2456202.453 | 0.003 | 5982 | 0.004 |
36 | 2455900.164 | 0.002 | 960 | 0.005 | 87 | 2456202.511 | 0.002 | 5983 | 0.002 |
37 | 2455900.216 | 0.002 | 961 | -0.003 | 88 | 2456216.229 | 0.003 | 6211 | -0.004 |
38 | 2455900.279 | 0.003 | 962 | -0.001 | 89 | 2456216.296 | 0.003 | 6212 | 0.003 |
39 | 2455900.341 | 0.003 | 963 | 0.001 | 90 | 2456216.357 | 0.003 | 6213 | 0.004 |
40 | 2455900.398 | 0.003 | 964 | -0.002 | 91 | 2456216.412 | 0.002 | 6214 | -0.001 |
41 | 2455901.184 | 0.003 | 977 | 0.001 | 92 | 2456216.474 | 0.002 | 6215 | 0.001 |
42 | 2455901.242 | 0.004 | 978 | -0.001 | 93 | 2456216.536 | 0.002 | 6216 | 0.002 |
43 | 2455901.303 | 0.003 | 979 | 0.000 | 94 | 2456217.317 | 0.002 | 6229 | 0.001 |
44 | 2455901.363 | 0.003 | 980 | 0.000 | 95 | 2456217.376 | 0.003 | 6230 | 0.000 |
45 | 2455901.422 | 0.003 | 981 | -0.001 | 96 | 2456217.434 | 0.002 | 6231 | -0.003 |
46 | 2455925.268 | 0.002 | 1377 | 0.008 | 97 | 2456217.498 | 0.002 | 6232 | 0.001 |
47 | 2455926.291 | 0.004 | 1394 | 0.008 | 98 | 2456218.342 | 0.002 | 6246 | 0.003 |
48 | 2455956.197 | 0.002 | 1891 | -0.002 | 99 | 2456218.403 | 0.002 | 6247 | 0.003 |
49 | 2456153.397 | 0.002 | 5167 | 0.006 | 100 | 2456218.459 | 0.002 | 6248 | -0.001 |
50 | 2456174.461 | 0.002 | 5517 | 0.002 | 101 | 2456218.521 | 0.002 | 6249 | 0.001 |
51 | 2456174.519 | 0.002 | 5518 | 0.000 | |||||
The light elements of the pulsations are:
Having 101 maxima observed on a time span of 392 days,
corresponding to 6249 pulsation cycles, we can fully explore
possible variation of the pulsation period of the Scuti
component, starting with the light elements (2). We calculated
pulsation maxima and determined
residuals, also presented in
the corresponding column of Table 3. The
residuals suggest
no variations of the pulsation period.
Using the light elements (1) and (2), we plotted the four light curves shown in Fig. 2. They illustrate the photometric behavior of the system.
We hope that the present study will stimulate new observations of this interesting star.
Acknowledgements: We would like to thank S.V. Antipin and N.N. Samus for helpful discussions.
References:
Sokolovsky, K., Lebedev, A. 2005, in 12th Young Scientists' Conference on Astronomy and Space Physics, Kyiv, Ukraine, April 19-23, 2005, eds.: Simon, A.; Golovin, A., p.79
Kwee, K., van Woerden, H. 1956, Bulletin of the Astronomical Institutes of the Netherlands, 12, 464
Lafler, J., Kinman, T.D. 1965, Astrophys. J., Suppl. Ser., 11, 216
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Fig. 2. USNO-A2.0 1350-17086180 light curves. The upper left curve displays raw data with the orbital period; the upper right curve, raw data with the pulsation period; the bottom left curve, raw data with pulsations removed, folded with the orbital period; and the bottom right curve, raw data with eclipses removed, folded with the pulsation period. |