by Air Force Institute of Technology, Air University .
Written in English
Not believed to be a CIVINS (Civilian Institutions) title.A semi-empirical method for modelling the loss of electron fluxes in the earth's magnetosphere was developed. An equation for the integral-energy omnidirectional electron flux as a function of time and magnetic field strength was derived from pitch-angle diffusion : Roger S. Dewey. Electron scattering loss in Earth's inner magnetosphere: 1. Dominant physical processes. Abstract. Pitch angle diffusion rates due to Coulomb collisions and resonant interactions with plasmaspheric hiss, lightning‐induced whistlers and anthropogenic VLF transmissions are computed for inner magnetospheric by: But describing the loss of electrons is a challenging problem. One important population of inner magnetosphere plasma that is highly relevant for calculating electron losses, and one which our model—the Rice Convection Model-Equilibrium (RCM-E)—has neglected, is the cold plasma population of the plasmasphere. Abstract. Observations of electrostatic waves in the Earth’s magnetosphere which exhibited complex frequency banding related to harmonics of the electron gyrofrequency (“3/2 f ce emissions”) were first reported by Kennel et al (1). The authors also pointed out that, given the large amplitudes often attained by the waves (≳ 1 mV/m), electrons would be rapidly diffused Author: P. J. Christiansen, M. P. Gough, K. Rönnmark.
Highly relativistic electrons (3–10 MeV) at times are observed to populate the earth's magnetosphere near the geostationary orbit (r ∼ R E). Electron fluxes and energy spectra are shown which were measured by two high-energy electron sensor systems at R E from to the present. Large, persistent increases in this electron population were found to be . The dynamics of the pulsar is fixed by the magnetic dipole radiation that carries angular momentum and energy, which is compensated by angular momentum and rotational energy losses. Radiation losses Rotational Energy losses From these eqs and Size: 6MB. Electron density cm 3 He2+ density cm 3 Flow speed (nearly radial) km.s 1 Proton temperature K Electron temperature K Magnetic eld (induction) 7 10 9 tesla (T) Table 1: Observed Properties of the Solar Wind near the Orbit of the Earth (From Kivelson & Russel), The MagnetosphereFile Size: 3MB. Electronic books: Additional Physical Format: Print version: Jaynes, Allison N. Dynamic Loss of Earth's Radiation Belts: From Loss in the Magnetosphere to Particle Precipitation in the Atmosphere. San Diego: Elsevier, © Material Type: Document, Internet resource: Document Type: Internet Resource, Computer File: All Authors / Contributors.
Energetic Particle Losses From the Inner Magnetosphere Hannu E. J. Koskinen 23 A Numerical Study on the Resonant Scattering Process of Relativistic Electrons via Whistler-Mode Waves in the Outer Radiation Belt. This study aims to assess how well different electron loss models can account for the observed electron fluxes during a geomagnetic storm. Three models of electron losses due to interactions with magnetospheric waves are used in the flux calculations, and the results are then compared with fluxes observed by the Van Allen Probes : C. P. Ferradas, C. P. Ferradas, C. P. Ferradas, V. K. Jordanova, G. D. Reeves, B. A. Larsen. About Cookies, including instructions on how to turn off cookies if you wish to do so. By continuing to browse this site you agree to us using cookies as described in About Cookies.. Remove maintenance message. The Dynamic Loss of Earth's Radiation Belts: From Loss in the Magnetosphere to Particle Precipitation in the Atmosphere presents a timely review of data from various explorative missions, including the Van Allen Probes, the Magnetospheric Multiscale Mission (which aims to determine magnetopause losses), the completion of four BARREL balloon campaigns, and Format: Paperback.