... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

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• Extinction properties (transmitted radiation)
• Wavelength dependence
• Circular polarization: change of sign

... We will consider the rms, (K), for observations with a receiver of system temperature, T , frequency resolution, per polarization, and total integration time per observing cycle, . ... For ``in-band'' frequency switching, the line under investigation is always in the observing band. ... Position Switching or ``Out-of-Band'' Frequency Switching: Here the line is only observed for one half of the time, with noise being present all of the time. ...

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• Thesis Figures
• Example Observing Projects
• aostatus Observer's Display

... Future seminars . ... Relativistic magneto-active laser plasmas " . ... Generation of super-strong magnetic fields. ... This method is based on the observation of resonance interaction between the Landau levels in magnetic field and energy levels of plasma ions. ... The important peculiarity of the energy distribution of fast ions is their slow decreasing up to the energy of 1.4 MeV at the laser intensity of 2 10 18 W/cm 2 ; the effective temperature of fast ions is of the order of 350 keV. ...

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• Solar Energetic Particles
• The Solar Wind
• Magnetospheres and the Universe

... Site User's Guide (revised January 2015) . General Observing Information . ... An area map is available, as well as detailed directions from regional airports. ... APO does not recommend using GPS for directions to the site; please use the written directions below. ... APO/SDSS/NMSU Purchasing, Travel, Receiving, and Shipping Procedures . APO Site Safety Plan, V2.31 (current); APO Sprinkler and Shutter Procedures (pdf) . ... Roads to APO are all paved but are subject to heavy snow and ice. ...

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• Observers Instructions for filling out the ARCSAT nightlog
• Manastash Ridge Observatory Directions Page
• Information for Observers

The first indication that the sun might be emitting a "wind" came from comet tails , observed to point away from the Sun, whether the comet was approaching the Sun or whether it was moving away. ... Comet Halley, with plasma tail kink . ... Sunlight pressure cannot explain such behavior, but in 1943 Cuno Hoffmeister in Germany, and later Ludwig Biermann, proposed that apart from sunlight, the Sun also emitted a steady stream of particles, a "solar corpuscular radiation" which pushed the ions. ...

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• Energetic Particles
• Solar Energetic Particles
• Incoherent scatter [Oulu]

. ___________________________________________________________________ The Electronic Universe Project e-mail: nuts@moo.uoregon.edu

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• Power Spectrum of Galaxies
• ELECTRICITY GENERATION
• The Galaxy Gallery: Messier Objects

SPECTRUM ANALYZER OF MAGNETIC PHENOMENA SAMW . Spectrum analyzer allows onboard computation of electromagnetic waves spectra registered (observed) in the ionosphere and magnetosphere in the ELF/VLF frequency band. ... It consists of magnetic antenna, preamplifier, 16 bit sigma delta AD converter, DSP processor and telemetry interface. ... The channels of lower frequencies are averaged and transmitted with lower repetition rate so the telemetry volume is reduced. ... Dynamic range: 90 dB . ...

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• Publications of Astronomy and Space Physics Department

Next: ATCA Spectral Line Correlator Up: Spectral Line Data Reduction Previous: Spectral Line Data Reduction . Because of the Doppler effect, the observed frequency of a spectral line can be related to the radial velocity between the observer and the source. ... where v is the radial velocity, the observed frequency, the rest frequency, and c is the speed of light. ... Next: ATCA Spectral Line Correlator Up: Spectral Line Data Reduction Previous: Spectral Line Data Reduction Miriad manager . ...

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• LMC HII Region Luminosities versus Observed Ionizing Stars
• The Propagation of Cosmic Rays from the Vicinity of the Galactic Centre
• Source size measurement from observed quasar microlensing

... Magnetic fields, subatomic particles, etc., traveling in different directions fill the universe. Do they deflect or otherwise affect one another? If so, isnт??t the information we get from them distorted? ... Neutrino astronomy, which is still in its infancy, is attractive because neutrinos interact so weakly with matter that few of these distorting effects occur. Get instant access to subscriber content on Astronomy.com! ...

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• What is the Higgs particle? | Astronomy.com
• Everything around us is spinning: particles, planets, stars, galaxies. Why not
• Cosmic rays radiate radio waves | Astronomy.com

Lectures . ... Home Lectures Lecture Series 2010-2011 Lecture Series 2010-2011 ? Particle Physics at the LHC and Cosmology? by Michael Tuts . ... Lecture Series 2010-2011 . ... Beyond New York City . ... Observing Resources for Amateur Astronomers - Part 1: Beginning Observers . ... A History of the First Forty Years of the Amateur Astronomers Association . ... Amateur Astronomers Medal . ... 2016 Amateur Astronomers Association of New York Designed by Press Customizr Powered by . ...

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• High Line ? Solar Observing ? Amateur Astronomers Association of New York
• Central Park ? Solar Observing ? Amateur Astronomers Association of New York
• Lecture Series 2010-2011 ? ?Illuminating Dark Matter? by Neal Weiner ? Amateur

... Three SCANs were obtained, two were in the -x direction at a wavelengths of 1400 and 2700 and one was in the +y direction at 2700 . ... Models were created to match the GHRS 1400 (FOC F140M filter) and the 2700 (FOC F278M filter) observations, see Figure 38.1 in which model profiles are offset by one pixel. ... The 1400 scan starts to diverge from the FOC model at ~1.0 arcsec, while the 2700 scan tracks the FOC model scan out to a distance of ~1.4 arcsec before diverging from the model scan. ...

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• Stars as Observed in the Infrared
• A New Database of Observed Spectral Energy Distributions of Nearby Starburst
• HST Observer Monthly

... COMPUTER SIMULATION OF RADIOWAVE MULTIPLE SCATTERING EFFECTS IN IONOSPHERE USING MONTE-CARLO METHOD . ... Distribution of reflected radiation on the ground is computed. ... Such influence can be remarkable if the scattering is multiple, i.e. the optical thickness for the scattering process is considerably greater than a unit. ... Radiation energy transfer in the slab is modeled by distribution of some particles carring small portions of radiation energy. ... The isotropic plasma approximation is...

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• Scientific Directions Achievements

Photon/Particle Counting Image Measurement System : PIAS-TI . The PIAS-TI is an extremely sensitive image measurement device developed for imaging and quantification in ultimate levels with an extremely small number of photons, electrons and charged particles. ... The PIAS-TI is a measuring system that makes use of the technology of the photon counter to detect the input positions of individual photons or particles, and accumulate them to create an image. ...

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• The BSA SNRs Survey
• HyperLEDA documentation: compilation of cz measurements (a110)
• Doppler Shift

... Back to the Live Radiation Monitor Data The radiation monitor on board XMM-Newton registers the total count rate and basic spectral information on the background radiation impinging on the spacecraft and its scientific instruments. ... Counting of pulses for a selected energy band and above the low thresholds. ... Sensitivity: due to the electronic threshold, actually only electrons with energy greater than 130 keV and protons greater than 1.3 MeV can be measured by this unit. ...

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• XMM Science Objectives
• XMM-Newton Trainee Project 2004
• XMM-Newton OM Response Files Page

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

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• http://www.gao.spb.ru/english/as/j2014/presentations/guseva.pdf

Astronomers at Armagh Observatory observed the partial eclipse of the Sun on 29 March under unusually good conditions. ... The images, taken by astronomer Miruna Popescu, shows the eclipse as seen from the Armagh Observatory at around 11:30 (Summer Time) on 29th March, and the way it was observed by astronomer Apostolos Christou with a small portable telescope equipped with a filter to protect against the Sun's dangerous radiation. ... For more images from Armagh see: Miruna Popescu's Pages . ...

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• Broadening of Si VIII lines observed in the Solar polar coronal holes
• Armagh Observatory
• Leonid Reports

. Language [RU/EN] Search: . Home . UP . Research . Projects . Services . Info . News . Events . Personal . Archive . Ionosphere and radiowave propagation: structure . The main page . Information . Publications: . 2011 - 2015 . 2009 - 2010 . 2007 - 2008 . 2005 - 2006 . 2000 - 2004 . 1995 - 1999 . Participation in International symposiums and conferences: . 2013 - 2015 . 2011 - 2012 . 2009 - 2010 . 2007 - 2008 . 2005 - 2006 . 2002 - 2004 . N.V. Pushkov . 09/04/2016 23:52 MSK . webmaster@izmiran.ru .

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• The 14 July 2000 meter-wavelength dynamic radio spectrum
• Oct-Nov 2003: Radio
• CMEs and Space Weather

... References: %Observed energy levels (1 - 10): Edlen, 1983, Ph. ... 28, 51 % Observed energy levels (4,5): Feldman, Curdt, Landi , Wilhelm, 2000, ApJ, 544, 508 % Observed energy levels (11): from the spectrum of Acton et al 1985, ApJ, 291, 865 % Observed energy levels (12 - 16,25 - 26): Doschek et al 1973, J.Opt.Soc.Am, 63, 1463 % Observed energy levels (2s2.2p3.3d configuration): Fawcett Hayes, 1975, MNRAS, 170, 185 %theoretical energy levels : Landi , E., ...

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• Clumpy dust disks
• K-band Arcetri Obscured Supernova Search - Detected Supernovae

... The following charts/text are intended as tools for monitoring the Type Ia supernovae ( SNe ) event visually or photographically (utilizing telescope equipped CCD equipment).The files include: A replication of The Type Ia SNe , V- magnitude (with data point checks from other cited references)and color index (B-V) templete (to indicate a general color-related trend of the type Ia ... I believe this might help alleviate some of the problems involving the making of acceptable amateur light curves...

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• Contributions by amateurs: SN1996X.
• APOD: 2004 November 14 - Leonids Above Torre de la Guaita
• APOD: 2000 November 26 - Leonids Above Torre de la Guaita

Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

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• instruct
• The spectrograph design and the observing procedure
• SCORPIO: Direct images