Peremennye Zvezdy


Section: PZ: main journal

Другое Ross Variables Identified with Minor Planets
PZ, vol. 27, N 3 (28.04.2007) | B. G. Marsden / CFA

Of the 379 candidate variables listed by F.E. Ross during 1925 - 1931, 97 appear in the NSV catalogue, and 51 of these were recorded on a single night. Ross recognized that some of the single-nighters were likely to be minor planets, and a few years ago J.R. Bedient identified six such cases. The present author has identified nine further Ross objects as long-known minor planets.

Другое Variable Stars in NSVS Database I. 86 New Variables in Andromeda
PZ, vol. 27, N 2 (30.03.2007) | D. Dimitrov, V. Popov

A search for light curves with variability in the NSVS data was carried out in a 46 square-degree area in Andromeda. The field contains 51955 light curves. We found 136 variables, 86 of them were not known previously. Extrapolating the density of the variables in the field to the whole NSVS, the total number of variables in the survey is estimated to be 52000 - 61000.

Другое CCD B & V Photometry of the Young, Active, Late-type Star PZ Telescopii
PZ, vol. 27, N 1 (29.03.2007) | J. L. Innis, D. W. Coates, T. G. Kaye

We present new CCD B and V photometry, obtained at the Brightwater Observatory in June and July 2006, of PZ Telescopii (HD 174429), a young, rapidly rotating late-type star with an active chromosphere. The CCD data were collected with a short focal-length telescope, giving a field of view near 0.80 x 0.55 deg, so target and comparison stars could be observed simultaneously. A periodogram analysis of the PZ Tel data returned a value of 0.94 d, consistent with earlier photometry. We found the amplitude of variation was ~0.06 mag in B and V, with evidence for a small colour variation of between 0.01 and 0.02 mag, the star being redder when fainter. From a comparison with previously published photometry we find that the amplitude of V-light variation is amongst the smallest ever observed. There is an indication that there was a maximum in the long-term brightness level near V=8.28 around the year 2000, with the current data being several hundredths of a magnitude fainter.

Другое The Absorption Spectrum Variability of T Tauri
PZ, vol. 26, N 8 (10.11.2006) | N. Z. Ismailov, N. K. Guliev, A. A. Aliyeva

We present the results of our long-term homogeneous spectroscopy of T~Tau, the prototype T~Tauri star. We demonstrate that the star's absorption spectrum varies in time and is weakly correlated with variations of brightness and emission spectrum. With increasing intensities of emission lines, the veiling of the photospheric absorption decreases. It is suggested that the absorption-spectrum variations are due to variable additional emission superimposed on the photospheric spectrum and that the amount of veiling is inversely correlated with the emission-line strength in the spectrum of the star.

Другое Period Changes in the Algol-type Eclipsing Binary System TYC 1744 2329 1
PZ, vol. 26, N 7 (20.10.2006) | K. V. Sokolovsky, S. V. Antipin, S. A. Korotkiy

We present the discovery and the times of primary minima for the eclipsing binary TYC 1744 2329 1 = ASAS 003933+2730.5. Our CCD observations compared to times of minima derived from the archival photographic plates and from the NSVS and ASAS-3 data clearly show that the orbital period of the system is variable.

Другое GSC 7672:2238: a binary system near the Delta Scuti star AI Vel
PZ, vol. 26, N 6 (1.08.2006) | P. Pereira, J. M. Santos-Junior, D. A. Pilling, W. S. Cruz

We report the results of a photometric and spectroscopic study of an eclipsing binary star in the field of the Delta Scuti variable AI~Vel. Time-series CCD photometry was performed allowing almost complete phase coverage. Our period search gave an orbital period of 0.9719d. The light curve is typical of short-period Algol stars and suggests the presence of phase-related increase of brightness (φ=0.1-0.2) which can be due to mass transfer phenomena. Another possibility is the presence of a spotted region. Spectroscopic observation shows the Balmer Hα absorption line, typical of Algol systems with a transient or absent disc.

Другое The Emission Spectrum of T Tau in 1971-1979
PZ, vol. 26, N 5 (5.07.2006) | N. Z. Ismailov, N. K. Guliev, A. A. Aliyeva

We present the results of our long-time homogeneous low-resolution spectroscopy of T Tau, the prototype T Tauri star. We show that the star's spectral activity was different at different times of the observations and possibly was cyclic, with a many-year cycle. Variable emission activity in spectral lines at different brightness ranges was revealed. During the star's brightest state, equivalent widths of hydrogen emission lines show variations up to the factor of 5. The observed properties of the emission spectrum can be explained by the disk-accretion theory.

Другое The light curves of the type Ia Supernova 2004fu
PZ, vol. 26, N 4 (28.06.2006) | D. Y. Tsvetkov

CCD UBVRI photometry is presented for the type Ia supernova 2004fu in NGC 6949. The light and colour curves are typical for this class of objects, the absolute magnitude at maximum and decline rate are in agreement with the relationship between these parameters established for SNe Ia.

Другое Photometric observations of Supernovae 2000E, 2001B, 2001V, and 2001X
PZ, vol. 26, N 3 (25.03.2006) | D. Y. Tsvetkov

CCD BVRI photometry is presented for two type Ia supernovae 2000E and 2001V, for SN Ib 2001B and SN II-P 2001X. The parameters of light curves and absolute magnitudes at maximum light are estimated. It is shown that all four supernovae are typical for their classes considering the shape of their light curves and maximum luminosity.

Другое Photometric elements and stellar parameters for the contact binary RZ UMi
PZ, vol. 26, N 2 (25.03.2006) | P. Cauteren, P. Lampens, P. Wils

The contact binary RZ UMi was discovered by Goranskij (1982), who also attributed it to the W UMa class with a period of 0.33735283 days. No other observations of this star have been published since. We therefore re-observed RZ UMi at Beersel Hills Observatory on nine nights between May 2001 and March 2003. The instrument used was a 0.4 m Newtonian telescope, equipped first with a SBIG ST7E CCD camera (2001-2002) and later with a ST10 XME camera (2003). The 2001 observations are unfiltered. From 2002 onwards, a V filter according to the specifications of Bessell (1995) was used. The exposure times varied between 120 and 180 seconds. All images were reduced with the aperture photometry procedure of the Mira AP software package and darkframed and flatfielded according to standard procedures.

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