... Sun as a Source of Perturbation of Near-Earth Medium and Solar System Bodies. ... Tidal Influence of the Sun on the Earth. ... Structure of Solar Atmosphere. ... Observing Manifestations of Solar Activity. ... Forecasting of Solar Activity. ... Influence of Solar Activity on the Structure and Dynamics of Terrestrial Atmosphere. ... Problem of Mechanism of Solar-Troposphere Connections. ... Phenomenons in Auroral Zones of the Earth as a Result of the Sun Influence on the Terrestrial Atmosphere. ...

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• Solar Physics
• Physics of Heliosphere

... The Sun of our solar system is a typical star of intermediate size and luminosity. ... The Sun has a very complex surface magnetic field created by convective flow of the electrically conducting solar material. ... The escaping hot coronal plasma is called the solar wind . ... See the table below for the observed features above the Sun's surface. ... Chromospheric features . Coronal features . ... dense clouds of material suspended above the surface of the Sun by magnetic field line loops . ...

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... In collaborative work with David Garc?a Alvarez (an Observatory PhD student now at Harvard) and John Butler, an extensive study of the RS CVn binary HR1099 was completed leading to two papers; the first on Doppler imaging and the second on flare activity. Spectra for the Doppler imaging were taken at two different sites, Kitt Peak National Observatory (KPNO), Arizona, and Mount Stromlo Observatory (MSO), Australia, during the 1998 MUltiSIte COntinuous Spectroscopic (MUSICOS) campaign. ...

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... the time of observation . ... Observing the Changing Position of the Sun To Establish Cardinal Directions . ... Observations of the Sun's apparent movement across the sky and its pattern of rising and setting in the east and west horizon helped to establish the cardinal directions. ... The final stage of the Sun's return was marked by the observation that the Sun had reached its highest altitude when the full width of your mitted hand could fill the gap between the Sun and the horizon. ...

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• ASP: Good Astronomy Activities on the WWW
• ASP: Light Pollution

... These structures are best observed at somewhat high latitudes so that they can be compared with other datasets, such as IRAS and H-alpha, without contamination by unrelated gas along the line of sight. HI structures like this have never been mapped with high angular resolution and sensitivity because nearly all HI sky maps have been done with angular resolution 36 arcmin. ... Part of the observing run. ...

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• http://www.naic.edu/vscience/schedule/tpfiles/GoldstontagA2187tp.pdf
• Heiles Symposium Presentations
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... The observed distributions of stars of different ages and metallisities in the Z coordinate relative to Sun: (a) young ( t 3 Gyr) metall-rich ( [Fe/H] -0.13 ) stars; (b) young metal-poor ( [Fe/H]<-0.13 ) stars; (c) old ( 3 Gyr) metal-rich stars, and (d) old metal-poor stars. ... next figure | previous figure . ...

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• Mid Scales Role
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... Science Users Information > Science Activities > Science in Garching > Research Area: STELLAR STRUCTURE AND EVOLUTION . ... Reset view all 3 per page 5 per page 10 per page Sort by Title A-Z Title Z-A Date asc Date desc Research Topics Planets and Star Formation Stellar Structure and Evolution Stellar Populations Cosmology and the Early Universe Scientific Positions Faculty Fellows Scientists Students . ... Planets and Star Formation Stellar Populations Stellar Structure and Evolution Faculty . ...

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• ESO - Thesis Topic: Properties of kinematically decoupled structures in
• ESO - PhD Thesis Topics offered by ESO Faculty Members
• ESO - Thesis Topic: The dawn of planets: structure and evolution of

Solar High Resolution Studies . ... Solar Group . ... High Resolution Studies . Small Scale Activity . ... High resolution observations at different heights in the solar atmosphere have emphasized that there is no such thing as a "quiet" Sun (e.g. Schrijver et al., ... This, and the temporal coincidence of other signatures, supports the idea that microflares are indeed just miniature flares, but that one needs a very high resolution in order to observe them (Cauzzi et al., 2003, in preparation) . ...

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• Arcetri Solar Physics Group: Solar Polarimetry
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Next: About this document Up: FOC Image Restoration Using Previous: Mathematical Methodology . ... Use of a mask was required to ensure that the saturated data were ignored in the resultant restoration which these authors obtained with an observed PSF. ... Hollis and colleagues obtained two public domain FOC F/96 images of the binary system R Aquarii and an observed PSF both in the light of twice ionized oxygen which emits a spectral line at 5007 ?. ... These images are not identical in details, . ...

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• Using PSFs for Image Restoration
• Bad Pixels GPI Data Pipeline 1.0 documentation
• Andy Fruchter's Homepage

... Several of the tasks in the spectral package share a common set of parameters. ... Each task in the spectral package has a hidden parameter which points to the pkgpars parameter file. The parameters stored here include the observed data sets and the model descriptor, and instrument-specific parameters. ... The observed counts and error data set contained in the table file ( *_obs.tab ) produced by qpspec will be the input data for subsequent spectral tasks. ...

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• activities
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Databases (NSDC) of the Natural Planetary Satellites. ... NSDC: Database of astrometric observations of Natural Planetary Satellites . ... They are thoroughly looking for observations in different sources, creating their owndatabases which are then mostly inaccessible to other researchers. ... In the file "content" with explications, the reference is given to the data source as well as the bibliographic reference. ... Data sources. ... Why a specific bibliographic database for Natural satellites? ...

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Next: Radio pulse characteristics Up: An overview Previous: The structure of neutron . Typically Gauss for normal pulsars . Consistent with flux conservation during stellar collapse . ... Gravity dominates stellar structure . B field dominates exterior . Stellar surface is so small that observed emission is dominated by the magnetic field. ... Only field lines inside light cylinder are closed . Particles are constrained move along field lines . ...

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• Southern Cross Astrophysics Conference Series
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• ATNF Colloquium

... The first task assumes the searching for chemical composition and sizes of particles which give the wavelength dependence of the extinction efficiencies close to the observed dependence of . Figure 7: Wavelength dependence of the extinction efficiency factors for homogeneous spherical particles of different sizes consisting of astronomical silicate and amorphous carbon. The dashed segment shows the approximate wavelength dependence of the mean galactic extinction curve at optical wavelengths. ...

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• Silicate minerals
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RADIOASTROPHYSICAL DEPARTMENT • INSTITUTE OF SOLAR-TERRESTRIAL PHYSICS RAS SB . Support of activities at the Radio telescope General information Main characteristics of the Radio telescope Observing programs General view of the antenna array Main research areas Principle of generation of radio images Radio telescope 's beam Receiving systems Main characteristics of the base receiving-recording complex Calibrations Data archive and databases Publication of ... 9.4 GHz band. ...

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... M94 or NGc 4736 is an early type spiral galaxy with tightly would spiral structure and a dominant, luminous central bulge. ... This exposure was for 1724 seconds through A1 and B1. ... NGC 7789 is an open stellar cluster in the Galaxy. This exposure is 1351 seconds through B5. ... The Coma Cluster of galaxies was observed for 1850 seconds through the A1 filter. ... NGC 1313 A spiral galaxy in the Fornax Cluster and host of two recent supernova was observed for 1384 seconds through A1 and B5. ...

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• Astronomy HyperText Book: Stellar Evolution

... Data of obs. ... Reduced (Paper I) . NGC 0023 . VIII.1998 . ... NGC 0132 . ... Reduced . NGC 0157 . ... NGC 0615 . ... NGC 0753 . ... NGC 0945 . ... Bad data (clouds); . NGC 0972 . ... II.1998 . ... NGC 1024 . ... NGC 1058 . ... NGC 1073 . ... NGC 1084 . ... NGC 1134 . ... NGC 1637 . ... NGC 2276 . ... NGC 2608 . ... NGC 2964 . ... NGC 3184 . ... Bad data (low S/N) . NGC 3338 . ... Bad data (IFP failure) . NGC 3344 . ... Reduced (bad data) . ... Back to Project Vortex. ...

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• Laboratory of spectroscopy and photometry of extragalactic objects : Vortex1

RATAN-600 OBSERVATIONS OF MICROWAVE STRUCTURE OF THE QUIET SUN T.I. Kaltman, V.M. Bogo d, A.N. Korzhavin, S.Kh. ... A small-scaled structure with the size of 20-40 arc sec is regularly observed with RATAN-600 one-dimensional observations. ... The daily monitoring with RATAN-600 observations provides p ossibilities to regularly estimate a state of the quiet Sun by emission characteristics of microwave small-scaled structure and to trace rises of new centers of activities. ...

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• HyperLEDA: documentation
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• Radio survey for new compact HII regions

... Sun images . Magnetic storms online . ... Geomagnetic activity forecast . ... March : 2012 . ... No geomagnetic storms were observed for the past 3 hours Geomagnetic storms were observed for the past 24 hours . Magnetic storm of level G1 (minor) from 00:00 to 03:00 UT . Magnetic storm of level G2 (moderate) from 03:00 to 06:00 UT . Magnetic storm of level G3 (strong) from 06:00 to 09:00 UT . ... Last updated: March 10, 2012 00:00 UT . ... 7(499)132-65-96, Fax: +7(499)132-65-97 . ...

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• Magnetic storms online June 01, 2013
• Magnetic storms online June 23, 2015
• Magnetic storms online November 04, 2015

... DLTS . ... Deep Level Transient Spectroscopy ( DLTS ) is a unique and powerful tool for the study of electrically active defects (known as traps) in semiconductors. DLTS can be used in one of two modes of operation; with Schottky diodes or with p-n junctions. ... The capacitance transient is measured as a function of temperature (usually in the range from liquid nitrogen temperature to room temperature 300K or above). ...

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• Laboratory for Spectroscopy of Molecular Structures
• Laboratory of Real Structure of Crystals ISSP RAS
• LHPP ISSP RAS

The Solar spots - are the dark formations on the Sun's disk. ... The greatest observed spot is 100 thousand kilomiters. The spots are the places of the magnetic fields' getting out to the solar atmosphere. ... That's why they look so dark . ... The Solar convection zone is the layer with the thickness of 150 - 200 thousand kilomiters, situated under the photosphere; the substance of this layer being in convectional movement transformes the energy from inside the Sun's to its surface. ...

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