Next: Identification and Analysis of Binary Star Systems using Probability Theory . ... We present a computing code for modelling energy flux distributions, photometric indices and spectral line profiles of (non-)radially pulsating Main-Sequence stars. ... In the case of slowly rotating stars one can use the zero-rotation approximation to describe stellar pulsations. Such a model was used already by Cugier, Dziembowski & Pamyatnykh (1994) to study nonadiabatic observables of Cephei stars. ...

The central velocity dispersion represents the internal motions of the stars along a column crossing the center of a galaxy or star cluster. ... The catalogue of collected velocity dispersions may be accessed in HyperLeda. vdis is the velocity dispersion given in km/s. The velocity dispersion gives to some approximation the scale for the specific kinetic energy contained in in un-ordered motions and combined with the velocity of rotation it may give an estimate of the specific kinetic energy. ...

... Subject and Problems of Stellar Astronomy. ... Plane of Galaxy, Methods of Its Location Determination. ... Stars Distances. ... Other Methods of Stars Distances Determination. ... Tangential Velocities, Their Determination by Self-Motions. ... Determination of Solar Apex and Spatial Velocity by Radial and Spatial Velocities of Stars. ... Features of Orientation and Parameters of Peculiar Stellar Velocities Ellipsoid. ... General and Selective Light Absorption in Galaxy. ... Darc Clouds in Galaxy. ...

... The department was founded in late sixties by Prof. D.Ya.Martynov, who for many years was also the director of Sternberg Astronomical Institute. At present time, the head of the department is Prof. A.M.Cherepashchuk, a pupil of D.Ya.Martynov and his successor as the director of SAI. Since Prof. Martynov, the scientific activity of the department was primarily related to binary stars. ... The department consists of 15 members most of which have Ph.D. in Astrophysics. ...

. Next: Pulse Widths Up: Integrated and single pulse Previous: Integrated and single pulse . љ . Huge variations from pulse to pulse . Integrating several 100 forms a stable profile . Integrated profiles differ widely . Basic model includes core + cone . Slice in different ways to get various profiles . љ љ . Figure 54: Integrated pulse profiles . Jon Bell . Thu Dec 19 15:15:11 GMT 1996

Лаборатория Физики Звезд . ... Специальная астрофизическая обсерватория Российской академии наук . ... О лаборатории . ... Новые LBV звезды в галактике Туманность Андромеды .. Подробнее . Свидетельства сверхкритической аккреции на черную дыру в SS433 .. ... Сверхкритический аккреционный диск в SS433 .. ... Пространственная структура оболочки Новой V1494 Орла обнаружена на БТА .. ... Открыта новая LBV-звезда Галактики - двойник знаменитой LBV-звезды P Лебедя .. ...

Next: Introduction Up: Optical Interferometer Script Data Previous: ROCHE Contents . ... About AMOEBA . ... The Hierarchical Stellar Systems Model Format . Stellar models . ... Type 0 . Uniform disks . ... Miscellaneous stellar disks . ... Young stellar objects and disks . ... Fit scenarios . Single-lined spectroscopic binary . Double-lined spectroscopic binary . Single-lined spectroscopic binary with astrometric orbit . Triple with velocity curves of close pair . ...

... The design for the ALPACA receiver includes a parallactic rotator that can turn +/- 15 degrees about the center of the array. The plots show the parallatic rotation rates, and allowable integration times for 30degree rotation (.ps) ( .pdf ) . ... arecibo is at about 18:21:14. the leftmost set is 28 to 19 deg, the rightmost set is 08 to 17 deg. ... Page 2: parallactic rotation rate vs Hour Angle (in minutes). declination's 00:21:14 to 17:21:14 are plotted in 1 degree steps . ...

Next: Rotation Periods of ZAMS stars Previous: T Tauri Stars . ... The first attempts to directly measure periodic modulation of T Tauri stars occurred in the early 1980s. Rydgren & Vrba (1983) observed four PMS stars using photoelectric photometry over a period of seven consecutive photometric nights. ... Because the spot lifetime is much longer than the rotational period, the observed effect will be a modulation of the light from the star synchronously with the rotation period. ...

Magnetic Stars, 2011, pp. 215 ­ 219 Constant Magnetic Field of 1 CMa: Geometry or Slow Rotation? ... We report recent observations of the sharp­lined magnetic Cep pulsator 1 CMa (= HD 46328). ... The pro jected rotational velocity is constrained to be v sin i 15 km/s. 2 Magnetic Field and Rotational Perio d Longitudinal magnetic field measurements were inferred using the Least­Squares Deconvolution (LSD) with a line mask carefully customized to the spectrum of 1 CMa. ...

Modelling stellar magnetic fields using spectrum synthesis JD L 16/03/09 Leverhulme Lectures on Stellar Magnetism Basic idea of spectrum synthesis We have a spectrum from a star , and we want to extract as much information as possible from it Basic strategy: starting from basic physics, compute the spectrum expected for this star if it conforms to our theories Expected ... Leverhulme Lectures on Stellar Magnetism 16/03/09 ...