Interplanetary disturbances in the solar wind produced by density, temperature, or velocity pulses at 0.08 AU.
Abstract
Timedependent solutions of a onefluid model of the interplanetary medium are investigated. This set of unsteady hydrodynamic equations has been written in conservation form in order to apply the LaxWendroff method for the solution of this problem. The initial disturbance is specified by a pulse at 0.08 AU (astronomical units). Physically, this pulse can be interpreted as having been caused by a solar flare, surge, or any other solar disturbance. The equilibrium condition is determined to be the steady solution of the governing equations and represents the quiet solar wind. The results are presented in terms of density, temperature, and velocity profiles of the interplanetary gas flow at heliocentric distances up to 6 AU at several times. Also, the trajectories of disturbances for various initial pulses are shown. Finally, we have used some June 1972 interplanetary observational data to compare with these theoretical calculations. On the basis of these results, the effects of solar disturbances on the interplanetary environment (such as the generation of large nonlinear wave trains in the shocks' wakes) can be inferred.
 Publication:

Solar Physics
 Pub Date:
 July 1976
 DOI:
 10.1007/BF00221493
 Bibcode:
 1976SoPh...49..187W
 Keywords:

 Astronomical Models;
 Interplanetary Medium;
 Solar Activity Effects;
 Solar Flares;
 Solar Wind;
 Density Distribution;
 Gas Flow;
 Magnetohydrodynamic Stability;
 Plasma Density;
 PlasmaParticle Interactions;
 Rarefied Gas Dynamics;
 Temperature Distribution;
 Velocity Distribution;
 Astrophysics