Method of Determination of Ion Temperature by the Variations of Satellite Induced Ion Trap Currents and Estimate of the Upper Limit of Ion Temperature at Altitudes of 10,000 Kilometers and Higher According to Data of AES Electron-2

Ion temperature determination by variations of satellite induced ion trap currents - Electron 2 satellite measurements of ion temperatures in ionospher

Plasma measurements conducted in the vincinity of Venus on the spacecraft VENERA-4

Plasma flux measurements in vicinity of Venus by charged particle traps on Venera-4 spacecraf

The magnetic field of Mars estimated from the data of plasma measurements by Soviet artificial satellites of Mars

The dimensions of the obstacle forming the shock wave of Mars are estimated by use of electron trap data from Mars 2, 3, and 5. The mean altitude of the obstacle at the subsolar point can be convincingly explained if the obstacle is the magnetosphere of Mars. On the assumption that Mars has its own dipole magnetic field, the magnetic moment of Mars is estimated, Mm approximately equal to 2 x 10 to the twenty second power gs x cubic cu

Estimates of the Upper Limit of Ion Temperature in the 7000-30,000 Km Altitude Range According to Measurements Aboard AES ''elektron-2''

Elektron-2 measurements of upper limits of ion temperatures between 7000 and 30,000 k

The effect of the hot oxygen corona on the interaction of the solar wind with Venus

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/95142/1/grl3589.pd

Magnetic field and plasma inside and outside of the Martian magnetosphere

Simultaneous magnetic and plasma measurements, carried out by wide angle plasma detectors in the Mars environment, are compared in order to identify regions with significantly different physical properties. Magnetograms and ion spectra indicate changes in the magnetopause and magnetosphere of Mars that are associated with the dynamic pressure effect of the solar wind

High energy neutrino yields from astrophysical sources II: Magnetized sources

We calculate the yield of high energy neutrinos produced in astrophysical sources for arbitrary interaction depths $\tau_0$ and magnetic field strengths $B$. We take into account energy loss processes like synchrotron radiation and diffusion of charged particles in turbulent magnetic fields as well as the scattering of secondaries on background photons and the direct production of charm neutrinos. Meson-photon interactions are simulated with an extended version of the SOPHIA model. Diffusion leads to an increased path-length before protons leave the source of size R_s and therefore magnetized sources lose their transparency below the energy $E\sim 10^{18}{\rm eV} (R_s/{\rm pc}) (B/{\rm mG}) \tau_0^{1/\alpha}$, with $\alpha=1/3$ and 1 for Kolmogorov and Bohm diffusion, respectively. Moreover, the neutrino flux is suppressed above the energy where synchrotron energy losses become important for charged particles. As a consequence, the energy spectrum and the flavor composition of neutrinos are strongly modified both at low and high energies even for sources with \tau_0\lsim 1.Comment: 15 pages, 16 figure

The Venus ionosphere

Physical properties of the Venus ionosphere obtained by experiments on the US Pioneer Venus and the Soviet Venera missions are presented in the form of models suitable for inclusion in the Venus International Reference Atmosphere. The models comprise electron density (from 120 km), electron and ion temperatures, and relative ion abundance in the altitude range from 150 km to 1000 km for solar zenith angles from 0[deg] to 180[deg]. In addition, information on ion transport velocities, ionopause altitudes, and magnetic field characteristics of the Venus ionosphere, are presented in tabular or graphical form. Also discussed is the solar control of the physical properties of the Venus ionosphere.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/25872/1/0000435.pd