Physical nature of the low-speed solar wind

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In situ observations indicate that the low-speed wind is highly variable. It commonly originates on open field lines that thread coronal streamers in the vicinity of the magnetic equator, but transient ejections are also a source of low-speed flows on occasion. Close to the Sun a large flow shear probably is common at the interface between low- and high-speed flows. Near solar activity minimum low-speed flows are confined to a narrow band 40-45{degree} wide centered roughly on the solar equator, but near solar maximum low-speed flows may dominate at all heliographic latitudes.

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10 p.

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Gosling, J.T. September 1, 1996.

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Description

In situ observations indicate that the low-speed wind is highly variable. It commonly originates on open field lines that thread coronal streamers in the vicinity of the magnetic equator, but transient ejections are also a source of low-speed flows on occasion. Close to the Sun a large flow shear probably is common at the interface between low- and high-speed flows. Near solar activity minimum low-speed flows are confined to a narrow band 40-45{degree} wide centered roughly on the solar equator, but near solar maximum low-speed flows may dominate at all heliographic latitudes.

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10 p.

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OSTI as DE96012818

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  • Scientific basis for robotic exploration close to the sun, Marlboro, MA (United States), 15-18 Apr 1996

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  • Other: DE96012818
  • Report No.: LA-UR--96-2247
  • Report No.: CONF-9604161--2
  • Grant Number: W-7405-ENG-36
  • Office of Scientific & Technical Information Report Number: 282791
  • Archival Resource Key: ark:/67531/metadc667463

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  • September 1, 1996

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  • June 29, 2015, 9:42 p.m.

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  • Feb. 26, 2016, 3:14 p.m.

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Gosling, J.T. Physical nature of the low-speed solar wind, article, September 1, 1996; New Mexico. (digital.library.unt.edu/ark:/67531/metadc667463/: accessed September 24, 2017), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.