. 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.

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. ...

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_ | ...

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 ...

... 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. ...

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. ...

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 . ...

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. ...

... 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. ...

... 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. ...