Solar wind flows associated with hot heavy ions

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Solar wind heavy ion spectra measured with the Vela instrumentation have been studied with the goal of determining the solar origins of various solar wind structures which contain anomalously high ionization states. Since the ionization states freeze-in close to the sun they are good indicators of the plasma conditions in the low and intermediate corona. Heavy ion spectra from three different periods throughout the solar cycle have been analyzed. These data are consistent with freezing-in temperatures ranging from approx. 1.5 x 10/sup 6/ K to higher than 9 x 10/sup 6/. The spectra indicating hot coronal conditions occur in roughly ... continued below

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Pages: 58

Creation Information

Fenimore, E.E. May 1, 1980.

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Description

Solar wind heavy ion spectra measured with the Vela instrumentation have been studied with the goal of determining the solar origins of various solar wind structures which contain anomalously high ionization states. Since the ionization states freeze-in close to the sun they are good indicators of the plasma conditions in the low and intermediate corona. Heavy ion spectra from three different periods throughout the solar cycle have been analyzed. These data are consistent with freezing-in temperatures ranging from approx. 1.5 x 10/sup 6/ K to higher than 9 x 10/sup 6/. The spectra indicating hot coronal conditions occur in roughly 1/7 of all measurements and almost exclusively in postshock flows (PSFs), nonshock related helium abundance enhancements (HAEs), or noncompressive density enhancements (NCDEs). The PSFs and HAEs are both probably interplanetary manifestations of solar flares. The observation of several flare-related HAEs which were not preceded by an interplanetary shock suggests that the flare-heated plasma can evolve into the solar wind without producing a noticeable shock at 1 AU. The NCDEs with hot heavy ions differ from the PSF-HAEs in several ways implying that they evolve from events or places with lower temperatures and less energy than those associated with the flares, but with higher temperatures and densities than the quiet corona. Active regions, coronal mass ejections, and equatorial streamers are possible sources for the NCDEs with spectra indicating hot coronal conditions. These events owe their enhanced densities to coronal processes as opposed to interplanetary dynamical processes. Models of the solar wind expansion demonstrate how some NCDEs can have extreme, nonequilibrium ionization distributions.

Physical Description

Pages: 58

Notes

NTIS, PC A04/MF A01.

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  • Other Information: Thesis

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  • Report No.: LA-8344-T
  • Grant Number: W-7405-ENG-36
  • DOI: 10.2172/5450282 | External Link
  • Office of Scientific & Technical Information Report Number: 5450282
  • Archival Resource Key: ark:/67531/metadc1065025

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Office of Scientific & Technical Information Technical Reports

Reports, articles and other documents harvested from the Office of Scientific and Technical Information.

Office of Scientific and Technical Information (OSTI) is the Department of Energy (DOE) office that collects, preserves, and disseminates DOE-sponsored research and development (R&D) results that are the outcomes of R&D projects or other funded activities at DOE labs and facilities nationwide and grantees at universities and other institutions.

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Creation Date

  • May 1, 1980

Added to The UNT Digital Library

  • Feb. 4, 2018, 10:51 a.m.

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  • March 23, 2018, 1:07 p.m.

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Fenimore, E.E. Solar wind flows associated with hot heavy ions, report, May 1, 1980; United States. (digital.library.unt.edu/ark:/67531/metadc1065025/: accessed May 20, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.