A catalog of visual double and multiple stars with eclipsing components

A new catalog of visual double systems containing eclipsing binaries as one component is presented. The main purpose of this catalog is to compile a complete list of all known multiples of this variety, both for current analysis and to highlight those in need of additional observations. All available photometric and astrometric data were analyzed, resulting in new orbits for eight systems and new times of minimum light for a number of the eclipsing binaries. Some of the systems in the catalog have acceptable solutions for their visual orbits, although in most cases their orbital periods are too long for simultaneous analysis. Also included, however, are a number of systems which currently lack an orbital solution but which may be suitable for simultaneous analysis in the future.Comment: 15 pages, 8 figures, 4 tables, published in A

MOTIVATION FOR EDUCATION IN X, D.O.O.

Zanima me, kaj podjetja v današnjem času naredijo za motivacijo in izobraževanje svojih zaposlenih. Trenutno gospodarsko stanje v svetu močno vpliva na ljudi, njihovo počutje, pogled in razumevanje trenutnega dogajanja v njihovem delovnem okolju. V diplomskem delu bom to njihovo videnje skušal prikazati. V enem večjih podjetij v Sloveniji bom skušal pokazati različne občutke zaposlenih v proizvodnji in tistih v pisarnah.I wonder what the companies today do for motivation and education for their employees. The current economic situation in the world has a significant impact on people, their well-being, a view and understanding of current developments in their work area. In my diploma work I will try to show their view. In one of the major firms in Slovenia, I will try to show the different views of the people employed in the production area and those in the offices

Orbits of 10 interferometric binary systems calculated by using the improved Koval'skij method

Orbital elements are presented of 10 interferometric binary systems with no previous orbit determination: WDS 07143–2621 (FIN 323), WDS 12064–6543 (FIN 367Aa), WDS 12446–5717 (FIN 65), WDS 13320–6519 (FIN 369), WDS 13574–6229 (FIN 370), WDS 14189+5452 (CHR 137), WDS 14373–4608 (FIN 318 Aa), WDS 16115+0943 (FIN 354), WDS 17018–5108 (I 1306), WDS 17221–7007 (FIN 373). The method used (Koval'skij-Olević) is briefly described

New and recalculated orbital elements of 5 double stars

In this paper are given the orbital elements for the following five double stars: ADS 674 A921, ADS 2849 A1831BC, ADS 4002 McA18Aab, c, WDS 07269+2015 = CHARA 26 and ADS 6138 A2869, corresponding astrophysical quantities (C,H) and also masses and dynamical parallaxes for ADS 674, ADS 2849 and ADS 6138

A first and 11 recalculated orbits of double stars

We present the first orbit for the pair CHARA 130 as well as recalculated orbits for the following double stars: ADS 161, ADS 207, ADS 293, ADS 1393 ADS 2531, ADS 5707, ADS 6126, ADS 6532, ADS 6623, ADS 11247 and ADS 16914. Also, the comparison of obtained dynamical with the Hipparcos parallaxes is made

New orbital elements of 5 interferometric double stars

In this paper, for the first time, are presented elliptical and Thiel- Innes orbitatal elements for the following interferometric pairs: WDS 00416+2438 = WRH, WDS 03271+1845 = CHARA 10, WDS 04044+2406 = McA 13 Aa, WDS 17095+4047 = McA 45 and WDS 23019+4219 = o And Aa. For the pairs WDS 03271+1845 = CHARA 10 andWDS 04044+2406 = McA 13 Aa are calculated total masses and dynamical parallaxes which are compared with corresponding Hipparcos parallaxes

New orbital elements for 5 double stars

In this paper are presented recalculated elliptical and Thiel-Innes orbitatal elements for the following double stars: WDS05255-0033, WDS12272+2701, WDS 13336+2944 and WDS 21031+0132 (two versions). The elements of the pair WDS 06074+2640 = McA 25 are calculated for the first time

Orbits of 6 binaries

In this paper the orbits of binaries WDS 10093+2020 = A 2145, WDS 21074-0814 = BU 368 AB and WDS 22288-0001 = STF 2909 AB are recalculated because of significant deviations of more recent observations from the ephemerides. For binaries WDS 22384-0754 = A 2695, WDS 23474-7118 = FIN 375 Aa and WDS 23578+2508 = McA 76 the orbital elements are calculated for the first time

Dynamics of quadruple system Finsen 332 = ADS 11640 = HIP 92027 = WDS 18455+0530

In 1829 Struve discovered a double star denoted as STF 2375 AB later on. Its separation was 2". 2. It was noticed by Finsen from the Southern Observatory (Johannesburg) in 1953 that the components A and B are close binaries with separations about 0".15. The motion within this quadruple system - FIN 332 Aa and FIN 332 Bb - has been monitored from that time on. The data about the motion of these close binaries are analyzed by the present authors and the preliminary orbital elements are calculated for each of them. The dynamical parallax from the obtained period and the semi major axis for pair FIN 332 Bb agrees completely with that obtained from the Hipparcos program. In the case of FIN 332 Aa a somewhat higher parallax but within the error limits following from the errors of the period and semimajor axis, is obtained and it agrees with the parallax for FIN 332 Bb. The dynamical masses for the components of both systems are as expected for their spectral type A1V (all of them belong to the Main Sequence and here one uses Angelov’s (1993) relation). According to our results, the motion of both systems takes place approximately in the same plane, confirming thus some general properties already noticed in the case of multiple stars

Kinematics of a sample of visual double stars

The Hipparcos-Input Catalogue also contains about 8000 already known visual double stars. In the framework of this-project campaign, in addition to other parameters, were also determined the parallaxes π, as well as the polar coordinates ρ and θ for double stars. On the basis of a comparison of these data to those obtained earlier from the ground based measurements (WDS Catalogue) statistical examinations of a double-star sample (1' ≤ ρ ≥ 14') are performed. It is shown that an exceptionally good agreement exists of the statistical distribution Δθ/Δt of the sample as function of ρ(AU) and the curve θ = C(ρ)/ρ2 representing the II Kepler law