Computer Science – Sound
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..315s&link_type=abstract
Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 315
Computer Science
Sound
1
Solar Wind Plasma, Sources Of Solar Wind, Waves, Oscillations, And Instabilities In Plasmas And Intense Beams, Plasma Simulation
Scientific paper
We simulated the 1 D nonlinear time-evolution of high-amplitude Alfvén, slow and fast magnetoacustic waves in the solar wind propagating outward at different angles to the mean magnetic (spiral) field, using the expanding box model. The simulation results for Alfvén waves and fast magnetoacustic waves fit the observational constraints in the solar wind best, showing decreasing trends for energies and other rms-quantities due to expansion and the appearance of inward propagating waves as minor species in the wind. Inward propagating waves are generated by reflection of Alfvén waves propagating at large angles to the magnetic field or they coincide with the occurrence of compressible fluctuations. It is the generation of sound due to ponderomotive forces of the Alfvén wave which we can detect in the latter case. For slow magnetoacustic waves we find a kind of oscillation of the character of the wave between a sound wave and an Alfvén wave. This is the more, the slow magnetoacustic wave is close to a sound wave in the beginning. On the other hand, fast magnetoacustic waves are much more dissipated than the other wave-types and their general behaviour is close to the Alfvén. The normalized cross-helicity σc is close to one for Alfvén-waves and this quantity is decreasing slightly when density-fluctuations are generated. σc decreases significantly when the waves are close to perpendicular propagation. Then, the waves are close to quasi-static structures.
Grappin Roland
Schmidt Manuel J.
Velli M. M.
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