Observations of the solar wind speed near the sun

Details Observations of the solar wind speed near the sun Observations of the solar wind speed near the sun

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...61g&link_type=abstract

California Univ., International Solar Wind 8 Conference, p. 61

Computer Science

Sound

3

Electron Density Profiles, Line Of Sight, Scintillation, Solar Wind, Solar Wind Velocity, Magnetohydrodynamic Waves, Interplanetary Space, Plasma Density, Eiscat Radar System (Europe), Ulysses Mission, Sound Waves, Stellar Mass, Mathematical Models, Electron Scattering, Wave Scattering, Density Distribution

Scientific paper

Two-antenna scintillation (IPS) observations can provide accurate measurements of the velocity with which electron density fluctuations drift past the line of sight. We will present recent IPS measurements made with the EISCAT and VLBA arrays. It is common, particularly during declining activity. for the line of sight to pass through plasma with a wide range of speed. Therefore it is important to account for the line of sight integration. It is clear from ULYSSES measurements that the speed is bimodal in nature, i.e., either 'fast' or 'slow.' Thus it is not necessary to model a continuous velocity distribution - one need only locate the 'fast-slow' interface. In addition one must consider the possibility that the density fluctuations are moving with respect to the flow of particles. Alfven waves propagating through field-aligned density fluctuations can mimic a sound wave in this respect, so the apparent IPS velocity can be the flow speed plus the Alfven speed. In modeling the IPS it is important that the scattering be 'weak,' because the weak scattering model requires only 1 spatial parameter instead of 3. Furthermore the effect of multiple velocities in much more distinct in weak scattering. EISCAT can only operate near 933 MHz, which limits the observations to outside of 17R(solar mass). The VLBA is the only facility with the combination of high frequency operation and long baselines required to observe inside of 15R(solar mass). A simple bimodal model has been successfully used to interpret our IPS observations near the sun. Farther out interaction regions have built up significantly and a two speed model is no longer valid. An apparent deceleration in the fast polar wind is sometimes evident when compared to the ULYSSES observation. The density variance delta N2e in the fast wind appears to decrease from equator to pole.

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