... Dept. for Physics of Stars&Galaxies . ... Astronomical Calendar . ... History of MAO . ... БЂ“ 2013. ... Zakhozhay O. and Vorobyov E.I. The signatures of disk fragmentation in spectral energy distributions // Proceedings of the conference Hot Planets and Cool Stars, Garching, November 12-16, 2012. ... Zakhozhay O.V., Vorobyov E.I. Spectral energy distributions of fragmenting protostellar disks // Formation, detection, and characterization of extrasolar habitable planets Proceedings IAU Symposium No....

... 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. ...

ATNF Home . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Information & tools for observers . ... Australia Telescope Online Archive (ATOA) . ... ATCA | ... Visiting Parkes radio telescope . ... Parkes radio telescope webcam . ... The Australia Telescope National Facility Colloquium . ...

... X-ray (left) and magnetic field (right) evolution of an X-ray jet in coronal hole. ... In both coronal holes and quiet-Sun regions, all brightening events are associated with bipolar regions and caused by magnetic flux emergence followed by cancellation with the pre-existing and/or newly emerging magnetic flux. ... The dominant flux of the coronal hole form the largest concentration of magnetic flux in terms of size while the opposite polarity is distributed in small concentrations. ...

... We are using Canadian Galactic Plane Survey l 74.2њ, -3.6њ < b This poster gives preliminary results for a full-fledged analysis of the gas properties and distribution of HISA features in the CGPS. ... where T ON and T OFF are observed brightnesses on and off the HISA feature, T S is the spin or excitation temperature of the HISA gas, tau is its optical depth, T C is the continuum intensity, and p is the fraction of H I emission lying behind the HISA feature. ... GIF | ...

... The sky distribution of the BCGs from the HSS sample is shown in Fig. 6 together with BCGs from the SBS and Case surveys (Izotov et al. [ 1993b ]; Pustilnik et al. ... First, we compare the apparent magnitude distributions of the three samples. ... The similar behaviour of the faint end of the apparent magnitude distributions infers that the Northern BCG sample may have a similar completeness down to this limiting magnitude. ...

... V.V.Shevchenko, Sternberg State Astronomical Institute, Moscow University, Universitetsky 13, Moscow 119899, Russia, shev@sai.msu.ru . ... 1.Sternberg State Astronomical Institute, 119899, Moscow, Russia. shev@sai.msu.ru . ... V.V.Shevchenko, Sternberg State Astronomical Institute, Moscow University, Moscow 119992, Russia, shev@sai.msu.ru . ... 119992 Moscow, Russia; . ... 2Sternberg Astronomical Institute, Moscow University, Moscow, 119992, Russia, . ... Moscow, 119992, Russia shev@sai.msu.ru . ...

Next: Redshift Distribution Up: Sample Identification Previous: Previously Identified Sources . ... In Figure 3, we plot the redshift distribution of DXRBS FSRQs opposite that of the 1 Jy and S4 samples. In Figure 4, we plot the redshift distribution of DXRBS BL Lacs opposite the Slew and 1 Jy samples. ... The apparent deficit of objects at the very highest luminosities is a result of the smaller area of sky covered by DXRBS compared to, e.g., the Slew and 1 Jy samples. ...

... Translate Abstract . ... Structure and properties of IRC+10216 . ... AA(Stockholm Observatory, SE--133 36 Saltsj baden, Sweden), AB(Special Astrophysical Observatory, Nizhnij Arkhyz, Karachaevo-Cherkesia, 357147, Russia), AC(Max-Planck-Insitut f r Radioastronomie, Auf dem H gel 69, D--53121 Bonn, Germany), AD(Max-Planck-Insitut f r Radioastronomie, Auf dem H gel 69, D--53121 Bonn, Germany), AE(Max-Planck-Insitut f r Radioastronomie, Auf dem H gel 69, D--53121 Bonn, Germany) . ... Abstract Text . ...

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. Spectral Energy Distribution of the microquasar LS 5039. This is a composite: observations were not taken simultaneously. From Paredes, Bosch-Ramon, Romero, A , 451, 259 (2006).

Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...

... Future seminars . ... Influence of solar activity on wheat prices in the medieval England " . Dr. L. Poustilnik, Dr. G. Yomdin (Sea of Galilee Astrophysical Observatory, Jordan Valley College; Israel Space Weather Center, Israel Space Agency & Tel Aviv University, Israel ) . ... In the next step, we analyze a direct link between wheat prices and solar activity in the 17th Century, for which wheat prices and solar activity/cosmic ray intensity data (derived from 10Be isotope) are available. ...

... We present Very Large Array observations of the intermediate mass pre-main-sequence stars UX Ori and CQ Tau at 7mm, 3.6cm, and 6cm. ... Both stars are detected at 7mm but not at longer wavelengths, which confirms that the millimeter emission is dominated by dust. ... The observations do not spatially resolve the 7mm emission. ... The CQ Tau system exhibits a spectral index in the millimeter range of alpha_mm~2.6, consistent with values commonly found for disks around pre-main-sequence stars. ...

... The nebular spectra of SNeIa can be used to determine the mass, density, and distribution of the SN ejecta, and the distance and reddening to the SN. Synthetic spectra can very rapidly be computed in NLTE and compared to the observed ones. Given the relatively large number of parameters, it is convenient to explore the parameter space in an automated form. The nebular spectrum synthesis code can be run in parallel on a workstation cluster. ...