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UX Ret and CN Hyi: hipparcos photometry analysis

Wadhwa, Surjit S.; Zealey, William J.

We present an analysis of the Hipparcos photometry of the contact binary systems UX Ret and CN Hyi. The Wilson-Devinney code is employed to model the V band light curve for several fixed values of the mass ratio. From the quality-of-fit of the different solutions a final solution is derived for each system. Absolute values of the system are derive…

Astrometric Solution of the Multiple System Xy Leo

Erdem, Ahmet; Bakis, Volkan; Budding, Edwin +2 more

An astrometric solution, together with time of minimum analysis, has been made for the multiple system XY Leonis (HIP 49136) to identify the properties of the remote companion to the eclipsing pair (AB). From this solution, we derive the inclination of the wide orbit (AB-cd) as 94.4^∘± 0.2^∘, angle of nodes as 247.3^∘…

Proper motion study of the ROSAT selected WTTS candidates around Taurus-Auriga

LI, J. Z.

Astrometric study of the T Tauri stars (TTS) candidates and non-TTS X-ray sources around Tau-Aur [Li, Hu 132 (1998) 173], based on the Hipparcos and the ACT Reference Catalogue, is presented in this paper. The ROSAT selected X-ray sources are found to have complicated nature. A few of them are associated with the Tau-Aur or the Orion Star Forming …

Preliminary Analysis of <Emphasis Type="BoldItalic">V</Emphasis> and <Emphasis Type="BoldItalic">Hp</Emphasis> Light Curves of 26 Carbon Miras

MikulÁšek, Zdeněk; GrÁf, TomÁš

Light variations of a representative sample of 26 more or less periodically variable carbon stars were analyzed on the basis of 2220 individual observations made by the Hipparcos satellite and 33 544 visual observations listed in AFOEV and VSOLJ databases within the interval JD = 2 448 000 (1988) ±6 cycles. We found the osculating linear ephemerid…

An Outburst Detected in the Spectrum of Hd 6226

Šlechta, Miroslav; Škoda, Petr

HD 6226 is a bright binary Be star at visual magnitude 6.81 (Hipparcos database). The emission and absorption phases occur in cycles, which are probably not periodic. The suspected period of about 630 days (derived from photometric measurements) is not confirmed by our spectroscopic survey. The latest emission phase developed in the beginning of 2…