The Sun and Heliosphere at Solar Maximum

E. J. Smith, R. G. Marsden, A. Balogh, G. Gloeckler, J. Geiss, D. J. McComas, R. B. McKibben, R. J. MacDowall, L. J. Lanzerotti, N. Krupp, H. Krueger, M. Landgraf

Research output: Contribution to journalReview article

51 Scopus citations

Abstract

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.

Original languageEnglish (US)
Pages (from-to)1165-1169
Number of pages5
JournalScience
Volume302
Issue number5648
DOIs
StatePublished - Nov 14 2003

All Science Journal Classification (ASJC) codes

  • General

Fingerprint Dive into the research topics of 'The Sun and Heliosphere at Solar Maximum'. Together they form a unique fingerprint.

  • Cite this

    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. (2003). The Sun and Heliosphere at Solar Maximum. Science, 302(5648), 1165-1169. https://doi.org/10.1126/science.1086295