The Sun and Heliosphere at Solar Maximum

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.; Krüger, Harald; Landgraf, M.

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The Sun and Heliosphere at Solar Maximum

Smith, E. J., Marsden, R. G., Balogh, A., Gloeckler, G., Geiss, J., McComas, D. J., et al. (2003). The Sun and Heliosphere at Solar Maximum. Science, 302(5648), 1165-1169. Retrieved from http://www.sciencemag.org/.

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Item Permalink: https://hdl.handle.net/11858/00-001M-0000-0011-8DB7-7 Version Permalink: https://hdl.handle.net/11858/00-001M-0000-0011-8DB8-5

Genre: Journal Article

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Creators:
Smith, E. J.¹, Author
Marsden, R. G.¹, Author
Balogh, A.¹, Author
Gloeckler, G.¹, Author
Geiss, J.¹, Author
McComas, D. J.¹, Author
McKibben, R. B.¹, Author
MacDowall, R. J.¹, Author
Lanzerotti, L. J.¹, Author
Krupp, N.², Author
Krüger, Harald², Author
Landgraf, M.², Author

Affiliations:
1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA, Space Science Department of European Space Agency, European Space Technology Center, Postbus 299, 2200 AG Noordwijk, Netherlands, Blackett Laboratory, Imperial College, London SW7 2BZ, UK, Department of Physics, University of Maryland, College Park, MD 20742, USA, International Space Science Institute, CH-3012 Bern, Switzerland, Southwest Research Institute, San Antonio, TX 78238, USA, Institute for the Study of Earth, Oceans and Space, University of New Hampshire, Durham, NH 03824, USA, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA, Bell Laboratories, Lucent Technologies, Murray Hill, NJ 07974, USA, Center for Solar Terrestrial Research, New Jersey Institute of Technology, Newark, NJ 07021, USA, *Present address M. Landgraf: European Space Operations Center, 64293 Darmstadt, Germany., ou_persistent22
2Ralf Srama - Heidelberg Dust Group, Research Groups, MPI for Nuclear Physics, Max Planck Society, ou_907558

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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.

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Language(s): eng - English

Dates: Date issued: 2003-11-14

Publication Status: Issued

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Rev. Type: Peer

Identifiers: eDoc: 60359
URI: http://www.sciencemag.org/

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Title: Science

Source Genre: Journal

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Pages: - Volume / Issue: 302 (5648) Sequence Number: - Start / End Page: 1165 - 1169 Identifier: -