The Sun and Heliosphere at Solar Maximum
E. J. Smith,1
R. G. Marsden,2
A. Balogh,3
G. Gloeckler,4
J. Geiss,5
D. J. McComas,6
R. B. McKibben,7
R. J. MacDowall,8
L. J. Lanzerotti,9,10
N. Krupp,11
H. Krueger,12
M. Landgraf2*
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.
1 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
2 Space Science Department of European Space Agency, European Space Technology Center, Postbus 299, 2200 AG Noordwijk, Netherlands.
3 Blackett Laboratory, Imperial College, London SW7 2BZ, UK.
4 Department of Physics, University of Maryland, College Park, MD 20742, USA.
5 International Space Science Institute, CH-3012 Bern, Switzerland.
6 Southwest Research Institute, San Antonio, TX 78238, USA.
7 Institute for the Study of Earth, Oceans and Space, University of New Hampshire, Durham, NH 03824, USA.
8 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
9 Bell Laboratories, Lucent Technologies, Murray Hill, NJ 07974, USA.
10 Center for Solar Terrestrial Research, New Jersey Institute of Technology, Newark, NJ 07021, USA.
11 Max Planck Institute for Aeronomy, D 37191 Katlenburg-Lindau, Germany.
12 Max Planck Institute for Kernphysik, 69029 Heidelberg, Germany.
* Present address: European Space Operations Center, 64293 Darmstadt, Germany.
