Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..110l&link_type=abstract
SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 110-1
Astronomy and Astrophysics
Astronomy
1
Particle Emission, Solar Wind, Interplanetary Magnetic Fields, Solar Wind Plasma, Sources Of Solar Wind
Scientific paper
Evolution of the large-scale stream structure of the solar wind flow is studied in the main acceleration zone at 10 to 40 solar radii from the Sun. Three independent sets of the experimental data were used: observations of the radio wave scattering using the large radio telescopes of the Lebedev Physical Institute, white solar corona images obtained with the SOHO spacecraft, and solar magnetic field strength computed from J.Wilcox Solar Observatory data. The positions of the transonic region of the solar wind flow derived from the radio astronomical observations data were used as a parameter reflecting the intensity of the solar wind acceleration process. Correlation studies of these data with the magnetic field strength in the solar corona permit us to reveal several different types of the solar wind streams. The 1995-2000 data show important changes in the solar corona magnetic fields and corresponding changes of the solar wind flow.
Lotova N. A.
Obridko Vladimir N.
Vladimirsky K. V.
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