The Sun and Heliosphere at Solar Maximum

Authors

E. J. Smith, Jet Propulsion Laboratory
R. G. Marsden, ESTEC - European Space Research and Technology Centre
A. Balogh, Imperial College London
G. Gloeckler, College of Computer, Mathematical, & Natural Sciences
J. Geiss, International Space Science Institute
D. J. McComas, Southwest Research Institute
R. B. McKibben, University of New Hampshire Durham
R. J. MacDowall, NASA Goddard Space Flight Center
L. J. Lanzerotti, Nokia Bell Labs
N. Krupp, Max Planck Institute for Solar System Research
H. Krueger, Max-Planck-Institut für Kernphysik
M. Landgraf, ESTEC - European Space Research and Technology Centre

Document Type

Article

Publication Date

11-14-2003

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.

Identifier

0242666182 (Scopus)

Publication Title

Science

External Full Text Location

https://doi.org/10.1126/science.1086295

ISSN

00368075

First Page

1165

Last Page

1169

Issue

5648

Volume

302

Recommended Citation

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.; and Landgraf, M., "The Sun and Heliosphere at Solar Maximum" (2003). Faculty Publications. 13925.
https://digitalcommons.njit.edu/fac_pubs/13925