. The frequency of the spectral maximum f m of the gyrosynchrotron emission vs. the column density of accelerated electrons calculated according to Dulk & Marsh (1982). Curves are shown for various power-law indices ? el of the electron spectrum and magnetic field strengths B . The angle between the line of sight and the magnetic field is 45 degree.

Еще в разделе: (Показать все результаты (>904) - www.izmiran.rssi.ru/ )

Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...

Еще в разделе: (Показать все результаты (>107) - space.univ.kiev.ua/ )

Synchrotron Radiation Emission from relativistic electrons gyrating round magnetic field lines. ... Different spectrum ( - optically thick - optically thin #" ! ... Can calculate radiated power from Larmor's equation. dipole pattern Mildly Relativistic Electrons Even for , relativistic beaming changes emitted spectrum significantly. Depar ture from dipole pattern and spectrum no longer a single emission line. gf !e d c 'b a` Y X h Ultra-Relativistic Electrons: Synchrotron Radiation B e v v|| v_ | ...

Еще в разделе: (Показать все результаты (>2753) - www.mrao.cam.ac.uk/ )

• http://www.mrao.cam.ac.uk/~kjbg1/lectures/lect3.pdf
• http://www.mrao.cam.ac.uk/yerac/garcia/garcia.ps
• Relic radiolines of hydrogen at decimeter and meter wavelength band

Linear Acceleration Emission in Radio Pulsars Mohammad Rafat School of Physics University of Sydney Supervisors: D. B. Melrose and Q. Luo Outline Pulsars: basic introduction Pulsar magnetosphere : vacuum model , corotating model , oscillating model Pulsar Emission : radio (coherent), high energy (incoherent) Linear Acceleration Emission Common cartoon (Wikipedia) Magnetosphere models Vacuum ...

Еще в разделе: (Показать все результаты (>21427) - www.atnf.csiro.au/ )

• Programme - Abstract
• Acceleration efficiency
• Limits on particle energies by resonant inverse Compton scattering

... gradients dependencies on solar wind parameters and IMF; . ... fate of thermal plasma at the dayside magnetopause. velocity-dispersed injections of the thermal and superthermal ions from LLBL at cusp and cleft (lowest energy VDIS-2 events); . ... outer cusp processes, role of outer cusp indentation, plasma entry (laminar reconnection, turbulent diffusion, others), role of turbulent boundary layer; . how is the magnetosheath plasma heated near magnetopause and cusp? . ... cusp/cleft wave emissions. ...

Еще в разделе: (Показать все результаты (>1757) - www.cosmos.ru/ )

• The Acceleration of the Aurora
• Solar Energetic Particles
• Space Research Institute (IKI) Seminar

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. ...

Еще в разделе: (Показать все результаты (>939) - www.iki.rssi.ru/ )

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

The following files list line and continuum emissivities from the Arcetri Spectral Code. ... File format (html): File format for the continuum files . ... File format (html): File format for binned line emission files Line emission - The emissivity is given for individual transitions greater than 10 -31 erg cm 3 s -1 Choose the electron density: Ne = 10^2 Ne = 10^3 Ne = 10^4 Ne = 10^5 Ne = 10^6 Ne = 10^7 Ne = 10^8 Ne = 10^9 Ne = 10^10 Ne = 10^11 Ne = 10^12 Ne = 10^13 Ne = 10^14 . ...

Еще в разделе: (Показать все результаты (>8867) - www.arcetri.astro.it/ )

• The Arcetri Spectral Code - E.Landi and M.Landini (1998)
• The Arcetri Spectral Code - E.Landi and M.Landini (2002)
• The Arcetri Spectral Code - E.Landi and M.Landini (2001)

Most current theories for magnetospheric emission can be grouped into polar cap, outer gap, and nebular models. These models, at least in some cases, need not be mutually exclusive; the Crab pulsar (among others), for example, shows clear evidence for pulsed emission from the magnetosphere and unpulsed emission from the surrounding nebula. ... This suggestion is strengthened by observation of a distinct soft emission component, consistent with the cooling scenario, from several of these pulsars. ...

Еще в разделе: (Показать все результаты (>3748) - hea-www.harvard.edu/ )

• *xflux, hxflux* - Calculation of X-ray Flux
• The AstroStat Slog Blog Archive Differential Emission Measure [Eqn]

... The new emission line galaxies are listed in Table 2 containing the following information: . column 1: The object's IAU-type name with the prefix HS. ... This was not corrected in the figure shown in Appendix A. HS1214+3801 : This is seemingly a supergiant H II -region at the very rim of the nearby edge-on disc galaxy (SA(s)cd) NGC 4244 (V hel = 224 kms -1 and B T =10.88). ... To check this option one needs a detailed map of the NGC 4244 velocity field including HS 1214+3801. ...

Еще в разделе: (Показать все результаты (>1974) - www.sao.ru/ )

• Radio spectra JAVA interface.
• LEDA data base
• Flux Densities of Radio Sources at 2695 MHz

... 33, No. 1, pp. 62­71. i Formation of Power-Law Electron Spectra in Collapsing Magnetic Traps S. A. Bogachev 1 1* and B. V. Somov 2** Lebedev Institute of Physics, Russian Academy of Sciences, Leninski i pr. ... It is shown that if the electrons injected into the trap have a power-law spectrum, then their spectrum remains a power-law one with the same slope throughout the acceleration process for both the Fermi and betatron acceleration mechanisms. ... They do not coincide at energies below 20 keV. ...

Еще в разделе: (Показать все результаты (>19443) - www.tesis.lebedev.ru/ )

• http://www.tesis.lebedev.ru/docs/139.pdf
• http://www.tesis.lebedev.ru/en/docs/128.pdf
• http://www.tesis.lebedev.ru/en/docs/1536.pdf

... The absolute flux calibration of NICMOS will be calculated from observations of standard stars with known flux distributions F( ). ... In order to expand the set of IR standard stars in the appropriate flux range for NICMOS, M. Rieke, R. Thompson, and collaborators at the University of Arizona are making photometric observations of solar-analog stars, which will be used to normalize the solar spectrum to the observed IR magnitudes. ... Relative flux references accurate to 1.5% for standard...

Еще в разделе: (Показать все результаты (>14189) - www.stsci.edu/ )

• CLASH: An Innovative Survey to Place New Constraints on the Fundamental
• Power Spectral Analysis
• Target Count Rates

11 august 2014/Monday: Arriving, Registration . ... The variation of solar flare coronal X-ray source spatial properties. ... Melnikov V.F., Charikov Yu.E., Kudriavtsev I.V. Directivity of X-ray and gamma-ray emission from different parts of flaring magnetic loops. ... E., Melnikov V.F. Angular characteristics of polarization degree of hard X-ray emission from different parts of flaring magnetic loops. ... The thick target model and analytical calculations of the hard X-ray emission from solar flares. ...

Еще в разделе: (Показать все результаты (>292) - www.gao.spb.ru/ )

... Particle distribution: dN d - with =1- ln pcn ln g Electron-photon conversion e + _ + _ electron _ e e electron/ positron high- energy photon e+ positron -25 cm cross-section, 10 8 6 4 2 0.5 1.0 center-of-momentum energy , MeV (log scale) 2 e + _ Proton-neutron conversion cm cross-section, 10 proton u +2/3 2 -28 d -1/3 6 u +2/3 4 resonance _ u d d+1/3 -1/3 d u+2/3 +2/3 -1/3 2 150 340 center-of-momentum ... Does the peak (cut-off) energy decrease with observation angle? Not always. ...

Еще в разделе: (Показать все результаты (>304) - hea.iki.rssi.ru/ )

• http://hea.iki.rssi.ru/integral06/papers/D39_Hartmann02-29Jan07_19:13:43.pdf
• http://hea.iki.rssi.ru/conf/hea2007/presentations.orig/26.12.07/chernyakova.pdf
• http://hea.iki.rssi.ru/integral06/papers/D37_Tsang01-08Feb07_19:28:05.pdf

... The IDL users can call these codes by the CALL_EXTERNAL function with the following syntax: res=CALL_EXTERNAL(libname, 'GET_MW', ParmIn, s, /F_VALUE) Here libname is the name of the appropriate dynamic link library or shared ob ject. ... Then, ParmIn is the 29-element single-precision floating-point array that contains the input parameters for the gyrosynchrotron code, and s is the two-dimensional single-precision floatingpoint array that contains the results of the computation. ...

Еще в разделе: (Показать все результаты (>2036) - star.arm.ac.uk/ )

• Astrodynamics 101
• Armagh Observatory

Proposal Identification No.: ... Proposal Type: General Category: Sub-Category: Observation Category: Total Time Requested: Minimum Useful Time: Prop osal Title: ABSTRACT: Urgent Astronomy Optical Thermosphere 10 Hours 3 Ionospheric modification using dual-frequency S-band beat modulation We attempt to create accelerated electrons near the F2 peak using S-band transmission of two frequencies separated by a frequency close to the critical ionopsheric frequency, fof2. ...

Еще в разделе: (Показать все результаты (>5064) - www.naic.edu/ )

• NVIDIA Accelerated Linux Graphics Driver README and Installation Guide
• Spectral-Line Observing
• Chapter 1. Introduction

XMM-Newton Science Analysis System Page: 1 rgscombine Jenny Carter (XMM-Newton SOC, jenny.carter@sciops.esa.int) (updated by CG) May 10 2007 Abstract Combines a list of spectrum les to create one combined spectrum le, and the corresponding list of response matrices and background spectrum , to create one nal response matrix and background ... Spectra can be in COUNTS or RATE (as produced by rgsbkgmodel) lepha no le The le name for the output combined spectrum. ...

Еще в разделе: (Показать все результаты (>6885) - xmm.vilspa.esa.es/ )

• Parallel detection over bands (with no assumptions made about source spectrum)
• Procedure

... The Galactic low-mass X-ray binary GS 2023+338 was discovered during the burst on May 22, 1989 with the Japanise satellite Ginga (aka Galaxy). The flux reached 17 crabs (this unit of flux measurement is an bright X-ray source, Crab Nebula) at 10-35 keV. ... No other radio telescope worldwide carried out multi-frequency measurements. ... Upon 14 days the radio flux fell below the detection level at the RATAN-600 in relation to the decrease of the X-ray flux. ...

Еще в разделе: (Показать все результаты (>263) - mavr.sao.ru/ )

• Detection of polarized radiation sources with unusual spectral characteristics
• Measurement of the dark halo shape in polar ring galaxies
• Speckle interferometry of magnetic stars

New RRC variables with an additional non-radial pulsation . PZ, vol. ... We present a new study of 14 known RR Lyrae variable stars from the Catalina surveys periodic variable star catalog. ... New Double-Mode RR Lyrae Variables III . ... We present a new study of 123 known RR Lyrae variable stars from the Catalina surveys periodic variable star catalog. ... According to these data, the stars are double-mode RR Lyrae variables, pulsating in the first-overtone and fundamental modes. ...

Еще в разделе: (Показать все результаты (>54989) - www.astronet.ru/ )

• XWare > APOD

... Research objects and scientific purposes . Space scientific program includes development and launch of two supersmall spacecrafts "Universitetskiy" and "Kompas-2" intended for monitoring of radiation conditions near the Earth. ... All the studies conducted in the near-Earth space are characterised by strong radiation fields. ... The circular polar orbits, which cover all the near-Earth space, are the most favorable for comprehensive studies of the radiation conditions near the Earth. ...

Еще в разделе: (Показать все результаты (>44) - cosmos.msu.ru/ )

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

Еще в разделе: (Показать все результаты (>516) - xray.sai.msu.ru/ )

• Frequency distribution of galactic binaries
• Effect of sources evolution on
• ADS Abstract Service Results