... A new study using AAT ?chelle spectroscopy and HST spectrophotometry has revised this value upwards to (Woolf & Jeffery 2000). Measuring for the PVTel variables poses considerable difficulties. ... In spite of these constraints, Jeffery et al. (2000) succeeded in obtaining nearly contiguous ultraviolet photometry and radial velocities ( ) of three PVTel variables. Analysis of the UV photometry provided measures of and . ... 2000). ...

We present Spitzer observations of the nearby dwarf starburst galaxy NGC 1705 obtained as part of the Spitzer Infrared Nearby Galaxies Survey. ... The nebular metallicity of NGC 1705 falls at the transition level of ~0.35 Zsolar found by Engelbracht and collaborators, below which PAH emission is difficult to detect; the fact that a system at this metallicity shows spatially variable PAH emission demonstrates the complexity of interpreting diffuse 8 О?m emission in galaxies. ...

... 371Gregory Taylor . ... We persent a catalog of 1274 discrete sources detected during a 5 yr, 6 cm, radio-patrol survey of the galactic plane for variavle sources. ... Seventy-five percent of the sources are weaker than 75 mJy, and as a consequence reliable sources and 27 possible variables were detected, of which 64 % exhibited shirt-term variability. ... A comparison with previous centimeter variability studies suggests the possible existence of two distinnct variability components. ...

Peremennye Zvezdy ( Variable Stars ) 32 , No. ... We report on our photometric analysis of the poorly studied cataclysmic variable in Ophiuchus, 1RXS J174320.1-042953 (DDE 11). ... The long-term behavior of J1743-0429 shows that it is a probable magnetic cataclysmic variable (polar), with a large difference between its low and high states. The orbital period obtained from our observations is 0 0866, or 2 08, close to the lower boundary of the period gap of cataclysmic variables. ... Fig. ...

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

... In nearly all cases, rgssources requires information from the CCF. ... Because the exceptions are insignificant and involve complicated logic to disentangle, it has been made mandatory to supply a CCF to the task. The location of the CCF is pointed to in the usual way, ie via the environment variable SAS_CCF. ... The task may also require information from the ODF summary file, in which case the variable SAS_ODF must be set before running the task. ...

... CEPHEID VARIABLE STARS: A Cepheid variable or Cepheid is a member of a particular class of very luminous, massive variable stars with pulsation periods of 1-70 days. ... The relationship is calibrated using data collected from Cepheids whose distances are determined by other means. ... Browse through the 68 CCD fits images he sent you, using ds9 and locate the Cepheid variable. ... Image credits: ESA - "http://sci.esa.int/science-e-media/img/20/cepheid-variables.jpg" . ...

Magnetic Stars, 2011, pp. ... In this paper we describe the reduction and analysis of the data, the constraints obtained on any magnetic field present in the stellar photosphere, and the variability of photospheric and wind lines. Key words: stars: early type ­ stars: supergiants ­ stars: magnetic fields ­ stars: winds ­ spectropolarimetry 1 Intro duction Rigel: a blue supergiant, the closest and most readily studied Type II supernova progenitor, and a known Cygni variable. ... 2008). ...

... We present a new method for visualizing flux variations in X-ray images. ... The time variability image so constructed visually shows area where strong time variation occurred. ... Figure 1. shows the intensity (left) and time variability (right) image of the ROSAT field centered on the X-ray source MKW 3. ... The corresponding time variability image is shown to the right. ... These examples clearly show the power of the method described in evidencing variable sources in crowded X-ray images. ...

The ESA/ESO Astronomy Exercise Series 2 . The Distance to Messier 100 as Determined by Cepheid Variable Stars . ... The small variations in distance to the individual Cepheid variable stars in the Cloud are negligible compared with the much larger distance to the SMC. ... In this way Cepheid variable stars can be used as one of the 'standard candles' in the Universe that act either as distance indicators themselves or can be used to calibrate (or set the zero point for) other distance indicators. ...

Follow-up observations with the University of Washington 0.76 m telescope at Manastash Ridge Observatory (MRO) of the Sloan Digital Sky Survey (SDSS) cataclysmic variable (CV) SDSS J170053+400358 are presented. ... They estimate that the dimming amounted to about 0.028 mag (using two comparison stars that were each about 4 mag fainter than HD 209458). only UW affiliated authors have been listed, student researchers are marked with an ``*'' . ... XTE J1859+226" UW affiliated authors: *Kevin Krisciunas. ...

... Astrophysics Group . ... COAST . COAST Astronomical Results . ... Surface Imaging of Betelgeuse . ... This page highlights some astronomical results obtained with COAST over the years. These are listed in chronological order (most recent first). ... Measurements of cyclic variations in the angular diameter of Chi Cygni . ... The first infrared image from an aperture synthesis array . ... The images of Betelgeuse below were reconstructed from COAST data taken in early 2004. ...

... INTRODUCTIO N Th e discovery of a strong variable surface magnetic field CrB, HD 126515 and 53 Cam (B ) in four Ap stars: HD 215441, (Preston, 1969a; Wolff and Wolff, 1970; Preston, 1970; Huchra, 1972) changed our knowledge about magnetic field geometry, formerly based only on effective field measurements (B ) . ... In this paper we present some results of an investigation of the variation with the rotation of the surface magnetic field for the Ap star 78 Vir using the curve of growth method. ...

We report first results of a multifrequency campaign from radio to hard X-ray energies of the prominent gamma-ray blazar 3C 279 during the first year of the INTEGRAL mission. The variable blazar was found at a low activity level, but was detected by all participating instruments. Subsequently a multifrequency spectrum could be compiled. ... In addition, this 2003 broadband spectrum is compared to one measured in 1999 during a high activity period of 3C 279. | ...

... There are preliminary series of photometric and radio spectral observations of the above-mentioned stars, archival data on the light curves of the stars, results of the search for OH and H 2 O maser emission in IRAS point sources that possess the IR parameters similar to Miras. ... The aim is a detailed study of the maser emission variability. ... In 1996-1997, astronomical observations of Mira Ceti-type stars (miras) were carried out in three spectral ranges: optical, infrared, and radio. ...

... The integration time (INT_TIME) is defined as the length of time over which the data were averaged to yield the given data point. ... Taking the system variable !int_time to specify an upper limit for the integration time in seconds which will not require integrating the model visibilities, will compare the actual integration times to this limit and determine the maximum number of computations required to cover the largest integration interval. ...

. На главную страницу НМУ . [ Postscript (20K) | Zipped postscript (8K) ] . Голоморфные функции и отображения. Феномен Хартогса. Оболочки голоморфности. Голоморфная выпуклость. Многообразия Штейна. Псевдовыпуклость и плюрисубгармоничность. Решение $\bar d$-уравнения по Хермандеру. Топология многообразий Штейна по Элиашбергу и Гомпфу.

... PUL VLBI Analysis Center . ... Pulkovo EOP and Reference Systems Analysis Center (PERSAC) is located at the Pulkovo Observatory . ... Processing of VLBI , GPS, and optical observations aimed at analysis of the Earth rotation, station displacement, and celestial reference system. ... Celestial Pole Offset (CPO) and Free Core Nutation (FCN) . Four daily updated CPO and FCN series (models) are provided. ... File fcn1.dat contains the ZM1 FCN model with variable amplitude and phase. ...

STEP INTO THE BLUE - MEADE INSTRUMENTS PRODUCT GUIDE . ... Telescopes . ... Superb optical performance coupled with time proven computerized pointing and tracking has made the LX200 ACF series a best-seller in the high-performance telescope class. ... General Accessories . ... Variable Projection Tele-Extender . ... The Meade 07348 Variable Projection Tele-Extender for LX Models requires the Meade 07182 eyepiece holder and offers different focal ratios while creating eyepiece-projection photography. ...

... R.A. = 00h55m04s.86, Decl. = -37 41'43".7 . ... Variable star in NGC 1511 . ... Variable star near Pegasus 2001bn IAUC 8624 BV anon 2001bh 7622 K star ugc11635 2001dh 7482 M star ic5374 1999db 7227 QSO anon 1999dc 7227 AGN anon 1999cx 7210 AGN anon 1999cu 7210 AGN anon 1999bs 7141 cat var ugc11093 1998di 6982 dwarf nova anon 1993U 5818 QSO anon 1993V 5818 QSO anon 1992W 5517 M star mcg 8-23-96 1992X 5517 M star mcg 6-32-24 1991ap 5327 QSO anon 1989Z 5162 var ngc4013 1985J 4059 CV ugc6274 ? ...