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  • SOLAR PHYSICS  (4)
  • 1985-1989  (4)
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  • 1
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    Solar wind observations with the ion composition instrument aboard the ISEE-3/ICE spacecraft (1989)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: The principal observations obtained by the Ion Composition Instrument (ICI) flown on the ISEE-3/ICE spacecraft, which was in the solar wind from September 1978 to the end of 1982, before being directed to the far magnetotail of the Earth are discussed. Almost continuous observations were made of the abundances of 3He++, 4He++, 06+, 07+, Ne, Si and Fe in various charge states, and of their bulk speeds and temperatures. The results show that there is a strong tendency in the collisionless solar wind for the ionic temperatures to be proportional to the masses. For heavier ions these temperatures exceed typical coronal electron temperatures. 4He++, especially in high speed streams, moves faster than H+, and travels at the same speed as heavier ions. The mechanism leading to this heating and rapid streaming is still not entirely clear.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 124; 1, 19; 167-183
    Format: text
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    NASA TECHNICAL REPORTS
  • 2
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    Coulomb collisions in the solar wind (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: A major improvement of the present investigation over previous studies of the subject is related to the use of helium temperatures obtained from helium ion measurements uncontaminated by the high-velocity tail of the proton distribution. More observations, covering a large parameter range, were employed, and the effects of interspecies drift were taken into account. It is shown in a more definite way than has been done previously, that Coulomb collisions provide the most important mechanism bringing about equilibrium between helium and protons in the solar wind. Other mechanisms may play some part in restricted regions, but Coulomb collisions are dominant on the macroscale.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 90; 7389-739
    Format: text
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    NASA TECHNICAL REPORTS
  • 3
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    Analysis of O(7+)/O(6+) observations in the solar wind (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: The ratio of O(7+)/O(6+) in the solar wind can be used to deduce the temperature at the point in the corona where the charge states become 'frozen' in the flow, and its determination therefore depends both upon the characteristics of the instrument and those of the source. The apparent increase of the ratio O(7+)/O(6+) observed in the solar wind by Ogilvie and Vogt (1980) at speeds above 450 km/s has been reevaluated using a greatly expanded data set. The ratio observed for solar wind speeds less than 450 km/s corresponds to an electron temperature of (1.7 + or - 0.2) x 10 to the 6th K in the region of 'freezing in' of the flow, as was previously reported. At higher speeds, when the kinetic temperature of the solar wind often exceeds (2-3) x 10 to the 5th K, instrumental effects become large and corrections difficult to determine.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 90; 9881-988
    Format: text
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  • 4
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    Solar wind observations with the ion composition instrument aboard the ISEE-3 ICE spacecraft (1989)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The principal observations obtained by the Ion Composition Instrument (ICI) flown on the ISEE-3/ICE spacecraft, which was in the solar wind from September 1978 to the end of 1982, before being directed to the far magnetotail of the Earth are discussed. Almost continuous observations were made of the abundances of 3He++, 4He++, O6+, O7+, Ne, Si and Fe in various charge states, and of their bulk speeds and temperatures. The results show that there is a strong tendency in the collisionless solar wind for the ionic temperatures to be proportional to the masses. For heavier ions these temperatures exceed typical coronal electron temperatures. 4He++, especially in high speed streams, moves faster than H+, and travels at the same speed as heavier ions. The mechanism leading to this heating and rapid streaming is still not entirely clear.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-101252 , NAS 1.15:101252
    Format: application/pdf
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