... This is one of the results from the Arecibo Methanol Maser Galactic Plane Survey that is being presented by graduate student Jagadheep D. Pandian of Cornell University, Ithaca, New York, Dr. Paul F. Goldsmith of Jet Propulsion Laboratory, Pasadena, California and Dr. Avinash A. Deshpande of Raman Research Institute, Bangalore, India to the American Astronomical Society meeting in Washington DC. ... Methanol masers at 6.7 GHz are beacons of massive star formation in our Galaxy. ...

... Research . ... A rare hybrid morphology radio galaxy . ... In this project we will be able to investigate the environmental effect on star formation and galaxy evolution in individual galaxies falling into the cluster through radio observations of active galactic nuclei (AGN). Current models of galaxy evolution regulate the star formation rates within the simulated galaxies by invoking radio-mode feedback from AGN. ... Julie.Banfield@anu.edu.au . ...

. Next: RGS_CLOCKPATTERNS Up: RGS_BADPIX Previous: References Contents . TEMPERAT= 1.63150000000000E+02 / [K] Temperature of CCDs OCB = 3 / On-chip binning factor . CCD_ID . NODE_ID . RAWX (pixel) . RAWY (pixel) . YLENGTH (pixel) . DESCRIPTION . TEMPERAT= 1.63150000000000E+02 / [K] Temperature of CCDs OCB = 1 / On-chip binning factor . CCD_ID . NODE_ID . RAWX (pixel) . RAWY (pixel) . YLENGTH (pixel) . DESCRIPTION . Michael Smith 2011-09-20

... Solar Wind . ... During a total eclipse of the Sun, when for a few minutes the Moon completely covers the Sun's face, a glow appears around the darkened Sun--the solar corona, the Sun's outermost atmosphere. ... Such high levels of ionization require the atoms to be buffeted around by extremely high temperatures, around 1,000,000 C (1,800,000 F). ... It is brightest near sunspots, whose arched field lines apparently hamper the outflow of solar wind which carries away energy and helps cool the corona...

... Solar Wind . ... During a total eclipse of the Sun, when for a few minutes the Moon completely covers the Sun's face, a glow appears around the darkened Sun--the solar corona, the Sun's outermost atmosphere. ... Such high levels of ionization require the atoms to be buffeted around by extremely high temperatures, around 1,000,000 C (1,800,000 F). ... It is brightest near sunspots, whose arched field lines apparently hamper the outflow of solar wind which carries away energy and helps cool the corona...

... My research focusses on spectral line and dust continuum observations of star formation in the Galaxy, particularly using the JCMT. My PhD thesis involved using HARP (the Heterodyne Array Receiver Project, see also my technical pages ), an array spectrograph built in the Cavendish Astrophysics Group for the James Clerk Maxwell Telescope ( JCMT ) for a wide-field survey of star formation. ... For an overview of the survey see Curtis, Richer Buckle (2010) . ... 2010) . ... 2010 Emily Curtis | ...

... In this section, we develop a physical model of the secondary as a disk that is centrifugally supported in the radial direction and hydrostatically supported in the vertical direction. We assume that the disk is vertically isothermal and well mixed. ... where is the mean molecular mass of the gas, is the orbital period at the outer edge of the disk in years, and all of the mass of the secondary has been assumed to be concentrated near its center, so the Keplerian approximation is valid. ...

... More than 300 surface reconstructions are already known for pure Si surface and Si surface with adsorbate. Study of their properties by the methods of surface physics reveal numerous interesting phenomena including various phase transitions accompanied by changes of Fermi-surface topology, development of the charge-density wave, etc . ... The charge-density wave (CDW) develops in materials with a chain-like crystal structure at temperatures below the Peierls transition temperature. ...

... Previous: Access to Atomic and Molecular Data/Databases in the VO . ... We present the general characteristics of a database for binary and multiple stars from all observational categories, specifically designed to address the awkward topics of the identification of stellar components. BDB is based on a modular architecture to allow the easy integration of data from various sources. We describe in particular the set up of connections with other double star databases through the Internet. ...

Two of the molecular clouds studied by Kainulainen and colleagues: The Pipe Nebula (left) and the Rho Ophiuchi cloud (right) in the Milky Way. In the background, an ordinary image of the Milky Way; each inset map shows to what extent the light of background stars is dimmed as it passes through the cloud in question. These maps form the basis of the 3-D reconstruction of cloud structure from which the astronomers derived their "recipe for star formation." ...

Properties of the interstellar gas clouds . ... The angular resolution of this Survey was 2.4' x 130', velocity resolution was 6.3 km/s, r.m.s. fluctuations of antenna temperature (T a ) was 0.25 K. All clouds with kinematical distances r a Some selection effects were discovered and our statistic results were corrected for them. Figure 1. ... In the very high mass range the number of neutral gas clouds may be decreased because of gravitational instability or/and molecularization. ...

... part 2 | ... Part 1 . The new concept of formation and development of the Solar system. ... Thus, the initial pulse of the rotation of a protosolar cloud of the solar system was determined as a result of the diversion of a part of the moment of the rotational pulse of the Galaxy. ... Besides this new approach to the pre-solar system as a system of the destroyed vortex structure, we can understand now a number of other peculiarities of the Solar system's structure. ...

... Ciel Espace, le magazine qui vous guide toujours plus loin . ... Ciel Espace, nouvelle formule, c'est . ... des pages consacr†йes †а la publication de vos photos Mais c'est aussi une vraie communaut†й avec laquelle partager votre passion et nourrir votre curiosit†й. Accueil DтАЩ†йtranges structures rocheuses sur Mars . ... Pour en savoir plus sur les explorations men†йes par Opportunity, †йcoutez le podcast Opportunity, †зa roule sur Mars , avec Fran†зois Forget, surle site cieletespaceradio.fr . ...

M87 Gas Disk and Optical Jet (STSci) . SEDS Messier Catalogue M87 Page (U. Arizona) . Black Hole and Jet in M87 (NASA/GSFC) . ... The large scale radio structure is shown in the 3CRR Atlas . Richard White's Virgo Cluster page has optical and X-ray images of the large-scale environment of M87 . ... HST Observes Distant Radio Galaxies (STScI) . HST Finds a Black Hole in NGC4261 (STScI) . HST finds a Bare Black Hole Pouring out Light in NGC6251 . ... Alan Bridle's Home Page . ...

... 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 . ...

... It is reasonable to expect that UV part of the irradiating spectrum is most influenced by the grain evolution (growth and sedimentation ) which marks the very initial stage of planet formation. 2 log J [erg s­1 cm­2] 1 0 -1 -2 -3 1000 BB 40 0 0 (A5 ) BB 20 0 00 (A5) Drai ne (A5 ) BP Ta u (A5) BB 40 0 0 (GS) BB 20 0 00 (GS) Drai ne (GS) BP Ta u (GS) Disk Model Density distribution is based on a 1+1D disk ... Green lines are used for a model with dust growth and sedimentation. ...

Observational Stellar Astronomy . Articles | ... We are made of star stuff" . ... TEMPERATURE OF A STAR: . ... The temperature of a star can be found out easily by simple observations. ... STAR . ... SPECTRAL CLASS: . All the stars in this universe are divided in to spectral classes based on their spectral lines. ... The spectral class of a star and the temperature of a star are related. So the spectral class can be found for a star since we know its temperature. ... www.astronomy.net . ...