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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: solar system |
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 |