The "ring of fire" seen by satellite cameras around the polar caps (picture below) is probably created by electrons leaking from the tail's plasma sheet, whose magnetic field lines form a somewhat imperfect trap. ... One possible explanation involves the close association between auroral arcs and electric currents which flow along field lines between the ionosphere and distant space ( Birkeland currents ). ... That produces an extra resistance to the flow of current. ...

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• Solar Energetic Particles
• Close-up of the Aurora
• Chronology of Magnetospheric Exploration

P. Frisch - Warm partially ionized interstellar gas at the Sun . ... W. M. Goss - Time variations in small-scale galactic HI structure toward 3C138 . S. Stanimirovic - Does tiny-scale atomic structure exist in the ISM? ... T. Bania - The distance to molecular clouds via HI self-absorption . ... C. Heiles - Arecibo Millennium Survey statistics of magnetic field, column density and turbulence in the CNM . R. Crutcher - Magnetic fields in molecular clouds . ...

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• Spectral-Line Observing
• Example Observing Projects
• CHVCs observed with Arecibo

... Magnetic Storms . ... Cosmic Rays . ... Energetic Particles . ... Solar fast Particles . We cannot observe the way the distant universe accelerates cosmic rays or produces energetic photons, but acceleration processes also occur on our Sun , though on a much more moderate scale. ... That is why such events are often missed by cosmic ray detectors near the equator, where the lowest energies are excluded by the Earth's magnetic field. ... Should we be concerned about solar energetic radiation? ...

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• The Acceleration of the Aurora
• Close-up of the Aurora
• Space Research Institute (IKI) Seminar

... Radiance image in Si iv 1402.8 (top-left, in reversed color table), Doppler velocity image (bottom-left), nonthermal velocity image (bottom-right) and HMI magnetogram (top-right) of region "A". ... The yellow box on the Doppler image outlines the region where anti-parallel flows are seen. ... A cluster of such loops was observed on the solar disk in active region NOAA11934, in the Si iv 1402.8 spectral raster and 1400 slit-jaw (SJ) images. ...

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• Small-Scale Dynamic Events in the Solar Atmosphere
• Solar Eclipse Observed Armagh Observatory
• Bright Point Studies

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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• The observed distribution
• Source size measurement from observed quasar microlensing
• LMC HII Region Luminosities versus Observed Ionizing Stars

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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• Fabry-Perot Interferometer: Gallery Old
• SCORPIO: IFP Gallery
• These galaxies were observed (Project: vortex)

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RADIOASTROPHYSICAL DEPARTMENT • INSTITUTE OF SOLAR-TERRESTRIAL PHYSICS RAS SB . Research results on fast active processes 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 ... Distribution of the recorded spikes in duration . ...

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A demonstration of HST WFPC image restoration has been made using both empirical and simulated PSFs. Empirical PSFs are obtained from the WFPC PSF library and also extracted from the image to be restored. Simulated PSFs are generated by the Tiny TIM package. The best results obtained thus far rely upon being able to determine a high S/N empirical PSF from the data frame. In order to achieve accurate restorations of data with high dynamic range excellent PSF models are required. ...

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• Stars as Observed in the Infrared
• Selected telescopes I have observed with
• Comparisons Between Observed and Model PSFs in WFPC Image . Restoration

... Science . ... Science Users Information > Science Activities > APEX Science Verification > SHFI . ... Observing Facilities . ... Observing with ESO Telescopes . ... Telescope Time Allocation . ... ESO Data . ... The Science Verification (SV) observations of the APEX Swedish Heterodyne Facility Instrument were observed in March 2008. ... A selection of the APEX-1 proposals listed below have been observed during the week of joint SV observations in March 2008, and later during the ESO time of period...

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• ESO - The Origin and Fate of the Sun: Evolution of Solar-mass Stars Observed
• ESO - Thesis Topic: Foreground emission and Cosmic Microwave background
• The globular cluster NGC 6388, observed by the NASA/ESA Hubble Space Telescope

... The TRACE images may be used without restrictions in publications of any kind. ... These two images, taken on 18 November 2000 at 15:54UT and 16:11UT, respectively, show such an event: the red circle in the image to the left shows a region where many loops are cooling, with bright loop tops (the intensity scales with the square root of the image to reduce the dynamic range). ... See also a collection of images related to the Sun, other cool stars, and solar-terrestrial effects . ... Images | ...

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• Procedures for Observations
• Clumpy dust disks
• CHIANTI atomic database

Solar Eruptive Event of 4 November 2001 observed with the SPIRIT Telescope on Board the CORONAS-F Satellite . ... Based on the data of the SPIRIT telescope on board the CORONAS-F satellite in three EUV channels 175, 284, 304 , we have analyzed large-scale manifestations of the post-eruptive so-lar activity followed one of the most considerable and geoeffective coronal mass ejection (CME) in the 23rd cycle which occurred on 4 November 2001. ... Posteruptive arcade on the CORONAS-F/SPIRIT movies at . ...

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• The 14 July 2000 meter-wavelength dynamic radio spectrum
• Ilya M
• magstorm

We report here on those proposed UIT targets that, in fact, were successfully acquired. ... Note on Filters: . A1 centered at 2500 angstroms with a width of 1200 angstroms . ... NGC 2300 is in a small group of galaxies which has a substantial amount of X-ray emission. ... LUNA again for 777 through lots of filters. ... Supernova 1987A in the Large Magellanic Cloud was observed for 3740 seconds through B5, A1 and B1. ... NGC 5128 or Cen A was observed for 1454 seconds through the B1 filter. ...

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... For observations we selected all Case galaxies in the zone = - from the Case lists III, IV, V, VIII, XI, XII and XIII which were classified in the Case survey by some indication on presense of [O III ] 4959,5007 emission lines (vs - very strong, s - strong, m - medium, w - weak, w? - weak?) and which had not been observed yet. ... Аdditionally nine Markarian galaxies in the same sky region were observed in hope to have better completeness in picking up all probable BCGs. ...

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• Emission-line galaxies
• The Hamburg/SAO Survey for Emission-Line Galaxies
• Results of follow-up spectroscopy

... Sun images . Magnetic storms online . Sun flares . ... September : 2015 . ... X-ray emission of the Sun from 08.09.2015 to 09.09.2015 (GOES-15) . No solar flares of C, M and X-class were observed today . No solar flares of C, M and X-class were observed yesterday . Last updated: September 10, 2015 00:00 UT . ... 1953-2016 Laboratory of X-ray astronomy of the Sun, LPI RAS, Russia . ... 7(499)132-65-96, Fax: +7(499)132-65-97 . ...

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• Solar flares online January 10, 2009
• Solar flares online January 10, 2011
• Solar flares online January 01, 2011

Emission Line Diagnostics in a ``No UV Bump'' Quasar PHL909 Smita Mathur, Belinda Wilkes, Martin Elvis and Jonathan McDowell Abstract PHL909 is a quasar with unusually low ultraviolet luminosity (blue bump strength C UV=IR = \Gamma0:20 compared to an average value of 0:4 (McDowell et al. ... The intrinsic continuum of PHL909 ( i.e. as seen by the BELR ) may thus be similar to the `standard' continuum, with a big blue bump, reddened along the line of sight. ...

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• http://hea-www.harvard.edu/PINTofALE/pro/flux_to_em.pro
• http://hea-www.harvard.edu/QEDT/Papers/STlines.ps
• Chandra Images for G120.1+01.4

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
• Researches of Astronomy and Space Physics Department

M. ( / DIAS, Ireland), A. (ISDC, Switzerland) 1 - Key Question Only 3 binary systems regularly observed in TeV: PSR B1259-63 (young pulsar +Be star, P=3.4 y) LSI +61 303 (comp. source + Be star, P=26.42 d) LS 5039 (comp. source + O star, P=3.9 d) Origin of the high-energy emission? ... 2006; Neronov &Chernyakova 2007 4 3.4 years orbital period. e~0.87 Correlated variability with a sharp rise ( "two bumps structure" ) is seen in radio, X-ray (and TeV?) bands. ...

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• http://hea.iki.rssi.ru/Z-90/arc/24/derishev.pdf
• http://hea.iki.rssi.ru/conf/hea2007/presentations.orig/25.12.07/medvedev.pdf
• http://hea.iki.rssi.ru/conf/hea2008/Presentations/24Dec/Chernyakova_IKI2008.pdf

... 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/publ-s/viii-rfs/p059.pdf
• http://www.gao.spb.ru/personal/ivanov/papers/ikhsanov2_2002.pdf
• http://www.gao.spb.ru/english/as/j2014/presentations/guseva.pdf

... Contacts . 2012: . ... We refined the fundamental parameters of the components, the orbital periods, and the conditions of photospheric heating of the secondary component by the ultraviolet radiation of the hot component. ... The observations of the star clusters associated with ultra-luminous x-ray sources (ULXs) in four galaxies on the 6-meter and VLT telescopes have shown that all the ULXs are located within 200pc of very young star clusters (younger than 5 million years). ... Archive . ...

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• Solar eclipse 2015
• Galaxy sector, archive 2008
• Ratan-600 schedule archive