The Sun and Heliosphere at Solar Maximum

Recent Ulysses observations from the Sun's equator to the poles reveal fundamental properties of the three-dimensional heliosphere at the maximum in solar activity. The heliospheric magnetic field originates from a magnetic dipole oriented nearly perpendicular to, instead of nearly parallel to,...

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Bibliographic Details
Published in:Science (American Association for the Advancement of Science) 2003-11, Vol.302 (5648), p.1165-1169
Main Authors: Smith, E. J., Marsden, R. G., Balogh, A., Gloeckler, G., Geiss, J., McComas, D. J., McKibben, R. B., MacDowall, R. J., Lanzerotti, L. J., Krupp, N., Krueger, H., Landgraf, M.
Format: Article
Language:English
Subjects:
Astronomy
Charged particles
Cosmic rays
Earth, ocean, space
Exact sciences and technology
Geophysics
Heliosphere
Magnetic fields
Magnetic flux
Magnetic polarity
Observations
Particle radiation, solar wind
Polar caps
Review
Solar energy
Solar flares
Solar physics
Solar system
Solar wind
Sun
Sunspots
Tropical regions
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Summary:Recent Ulysses observations from the Sun's equator to the poles reveal fundamental properties of the three-dimensional heliosphere at the maximum in solar activity. The heliospheric magnetic field originates from a magnetic dipole oriented nearly perpendicular to, instead of nearly parallel to, the Sun's rotation axis. Magnetic fields, solar wind, and energetic charged particles from low-latitude sources reach all latitudes, including the polar caps. The very fast high-latitude wind and polar coronal holes disappear and reappear together. Solar wind speed continues to be inversely correlated with coronal temperature. The cosmic ray flux is reduced symmetrically at all latitudes.
ISSN:0036-8075
1095-9203
DOI:10.1126/science.1086295