Andronov, I. L.

Ostrova, N.

Siwak, Michał

Winiarski, Maciej

Zoła, Stanisław

Information Bulletin on Variable Stars

English

Jagiellonian Univeristy Repository

COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARSNumber 5639Konkoly Observatory Budapest 2 August 2005HU ISSN 0374 -  0676DISCOVERY OF A N E W  PULSATING STAR: SAO 29875ZOLA, S.1-2; OSTROVA, N.3; SIWAK, M.1; WINIARSKI, M.1; ANDRONOV, I. L.3-41 Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Cracow, Poland, e-mail: sfzola@cyf-kr.edu.pl, siwak@oa.uj.edu.pl2 Mt. Suhora Observatory, Pedagogical University, ul. Podchorążych 2, 30-084 Cracow, Poland3 Department of Astronomy, Odessa National University, T.G. Schevtchenko Park, 65014 Odessa, Ukraine, e-mail: nataly_ostrova@mail.ru4 Crimean Astrophysical Observatory, UA 98409 Nauchny, UkraineName of the object:SAO 29875, HD 238549, BD+56 1883Equatorial coordinates: Equinox:R .A .=  10" 17”'3017 D E C .=  +56°14'19"9 2000Detector: photometer: three channel, Hamamatsu R1463P PMTsType of variability: A Boo/5 SetTransformed to a standard system: NoCheck star(s): noneComparison star(s): PG1618+563 used in March, anonymous star in AprilFilter (s): BVRObservatory and telescope:Mt. Suhora Observatory, 60 cm Cassegrain telescopeDate(s) of the observation(s):2005.03.20/21, 2005.03.21/22, 2005.044)273Availability of the data:Available at the IBVS website as 5 6 3 9 -t l.tx t2 IB VS 5639Remarks:We report discovery of pulsations of SAO 29875 (V=9^8, AO spectral type listed in the HD catalogue). In Fig. 1 we show the collected light curves in all filters. Variability with an amplitude of about 0^05 in B filter is clearly seen in the data collected in March. Although the April data have been gathered in non-photometric conditions, the light changes are obvious in all filters. SAO 29875 seems to have more than one periodicity as the observations taken during the first night show an increase of amplitude of pulsations towards the end of the run. We performed a Fourier analysis in order to search for periodicities. Deeming’s (1975) algorithm modified by Kurtz (1985) was applied. In Fig. 2 we present the periodogram for all available data taken in the B filter. Using the FOUR-M code (Andronov 1994), the value of the dominant period has been found: P=0.063656±0.000003 d. This dominant period is well seen every night. A longer-period peak of 0.315 d may have arisen as an artefact corresponding to the lengths of the runs (about 8 hours each night).The period and semi-amplitude properties of SAO 29875 may indicate either a 5 Set-type or A Boo-type pulsations. The A0 early spectral type may give a hint that SAO 29875 is a new A Boo-type pulsator. The final classification can be made after deriving the metal abundances of this star (Gray 1988, Paunzen 2005).Acknowledgements:N.O. would like to acknowledge the support from the Krolowa Jadwiga Jagiellonian University Fund.Figure 1. Light curve of SAO 29875IB VS 5639c/dFigure 2. The periodogram of all dataReferences:Andronov, I.L., 1994, Odessa Astron. Publ, 7, 49 Deeming, T.J., 1975, Astroph. & Sp. Sci., 36, 137 Gray, R.O., 1988, AJ, 95, 220 Kurtz, D.W., 1985, MNRAS, 213, 773 Paunzen, E., 2004, IAU Symp., 224, 443

Discovery of a new pulsating star : SAO 29875

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Discovery of a new pulsating star : SAO 29875

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