... Classes . ... classes that define a functional representation of the sky brightness More... class . casa::ComponentList . A class for manipulating groups of components. More... class . ... Base class for component shapes. ... Base class for model components of the sky brightness. ... A model component of the sky brightness. ... Base class for spectral models. ... Internal ComponentModels_module classes and functions. classes that define a functional representation of the sky brightness . ...

... Right: Schematic of disk reprocessing in X-ray pulsars. The hard (power-law spectrum) X-ray beam sweeps around and illuminates the accretion disk, which reradiates a soft X-ray (blackbody) component. ... X-ray binaries owe their prominence to one of the most efficient energy release mechanisms known: accretion onto a compact object. In the accretion process gas from the atmosphere of the less dense companion is accelerated toward the extremely dense compact star. ...

The night sky brightness, together with number of clear nights, seeing, transparency, photometric stability and humidity, are some of the most important parameters that qualify a site for front-line ground--based astronomy. ... Night sky at ESO-Paranal (Chile). ... Night sky brightness data . ... UBVRI night sky brightness at ESO-Paranal during sunspot maximum (A 2003, PDF) . ... The Dancing Sky: six years of night sky observations at Cerro Paranal (Starlight 2007 conference proceedings, PDF) . ...

... Minute Values of Geomagnetic Field Components . ... AA 1868 - Present (3 hourly and daily) (monthly) (yearly) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) KP_AP 1932 - Present (3 hourly and daily) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) AE_HV 1957-75, 78-88 (hourly) AE_MIN 1978-881-6;198903;1990-94 (minute) DST 1957 - Present (hourly) PC 1975 - Present (15-minute) AMANAS 1959 - Present (3 hourly and daily) KMKNKS 1983 - Present (3 hourly) . ...

A LINK BETWEEN VARIABLE OPTICAL CONTINUUM AND RADIO EMISSION OF A COMPACT JET IN THE RADIOнLOUD SEYFERT GALAXY 3C390.3 T.G. Arshakian 1 , A.P. Lobanov 1 , V.H. Chavushyan 2 , A.I. Shapovalova 3 , J.A. Zensus 1 , N.G. Bochkarev 4 , A.N. Burenkov 3 1 MaxнPlanckнInstitut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany, 2 Instituto Nacional de AstrofТРsica, Optica y ElectrТonica, Apartado Postal 51. ... We combine results from the monitoring of 3C390.3 in the optical region (Shapovalova et al. ...

... Flux density at 1 GHz (/Jy): 2720 . ... 1991, ApJ, 373, 146. ... ADS . ... VLA at 1.4 GHz and 4.8 GHz (both 1".3), for polarisation studies. ... VLA at 1.4 GHz and 4.8 GHz, for proper motion studies. ... 151 MHz observations for bulk expansion studies. ... Chandra observations, showing outer shock. ... Fesen et al. ... Spitzer observations. ... Chandra observations of rim. ... 2006, ApJ, 636, 848. ... 2006, ApJ, 647, L41. -ray line observations. ... Spitzer and Chandra observations for 3-D structure...

Общая Астрономическая Конференция . ... Правила форума . ... Сообщения за день . ... Добро пожаловать на Общая Астрономическая Конференция. ... Форумы общей направленности . Любые вопросы от новичков (просматривают: 17) . ... Общий форум любителей астрономии (просматривают: 7) . ... Новости магазина Starshop.ru . ... Менее астрономические товары (просматривают: 1) . ... Форум исключительно для сообщений об испытаниях астрономической техники. ... Общая Астрономическая Конференция статистика . ...

... Director of the RAS ISR . RAS Academician . ... Astrophysics module Kvant of the orbital complex Mir launched in 1987 contains the largest on the station complex of the scientific equipment named the orbital observatory Roentgen. Observatory Roentgen consists of 4 X-ray telescopes, jointly exceeding the range of energies from 2 to 800 keV. ... Among the most significant results that were received in the observatory Roentgen are: . ... measurement of the periods of 9 X-ray pulsars; . ...

... A new CLEAN-type algorithm searches for model components not in the dirty image but in the multi-resolution wavelet transform of the dirty image based on the dirty beam. A single-resolution prototype algorithm that searches for CLEAN components after convolution with the dirty beam has been tested and shown to be advantageous for the case of sparsely sampled and noisy u-v data, without specifying regions to be CLEANed. ... 530 Horiuchi, Kameno, and Ohishi CLEAN Wavelet CLEAN Figure 1. ...

Halo and Hexagons . ... In the foreground, the structure and individual component mirrors of Whipple's 10 meter gamma-ray telescope actually block direct light from the lunar disk, emphasizing the halo in this dramatic view. The halo was caused by ice crystals in the thin high clouds above the observatory - crystals that are hexagonal in shape and produce the characteristic ring of light with a 22 degree radius. ... NASA Web Site Statements, Warnings, and Disclaimers . ...

... 2006 November 9 . Halo and Hexagons . Credit Copyright: Gil Esquerdo ( Whipple Observatory ) . Explanation: As a bright November Moon lit up the night sky last week, Gil Esquerdo spotted this lovely Moon halo overhead at the Whipple Observatory on Mt. ... In the foreground, the structure and individual component mirrors of Whipple's 10 meter gamma-ray telescope actually block direct light from the lunar disk, emphasizing the halo in this dramatic view. ... About APOD | ...

Kholtygin A., Brown J., Fabrika S., Surkov A. Magnetic field connected fast line profile variability in spectra of bright O supergiants . ... Conference, held in the Special Astrophysical Observatory of the Russian AS, August 27-31, 2003, Eds.: Yu. ... Results of a study of fast line profile variability ( lpv ) in spectra of selected bright O-stars are reported. ... In the context of testing the MCWS model a program of searching for weak magnetic fields in bright O and early B stars is outlined. ...

Role in the Universe IAU Symposium 209, 2002 M. Dopita, S. Kwok and R.S. Sutherland, eds. Near-infrared monitoring of the carbon star IRC +10 216 : A high spatial-resolution time sequence of dust -shell evolution G. Weigelt , T. Blocker, K.-H. Hofmann, A. Men'shchikov, J.M. Winters Max{Planck{Institut fur Radioastronomie, 53121 Bonn, Germany Y. Balega Special Astrophysical Observatory, Nizhnij Arkhyz, 35147, Russia The carbon star IRC +10 ... 2000, Tuthill et al. 2000). ...