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

doi:10.1126/science.1086295

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 journal › Review article › peer-review

55 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 language	English (US)
Pages (from-to)	1165-1169
Number of pages	5
Journal	Science
Volume	302
Issue number	5648
DOIs	https://doi.org/10.1126/science.1086295
State	Published - Nov 14 2003
Externally published	Yes

All Science Journal Classification (ASJC) codes

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10.1126/science.1086295

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title = "The Sun and Heliosphere at Solar Maximum",

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.",

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

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doi = "10.1126/science.1086295",

language = "English (US)",

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T1 - The Sun and Heliosphere at Solar Maximum

AU - Smith, E. J.

AU - Marsden, R. G.

AU - Balogh, A.

AU - Gloeckler, G.

AU - Geiss, J.

AU - McComas, D. J.

AU - McKibben, R. B.

AU - MacDowall, R. J.

AU - Lanzerotti, L. J.

AU - Krupp, N.

AU - Krueger, H.

AU - Landgraf, M.

PY - 2003/11/14

Y1 - 2003/11/14

N2 - 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.

AB - 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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M3 - Review article

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SP - 1165

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JO - Science

JF - Science

IS - 5648

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The Sun and Heliosphere at Solar Maximum

Abstract

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