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  • 1
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    Solar wind composition from sector boundary crossings and coronal mass ejections (1992)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: Using the Ion Composition Instrument (ICI) on board the ISEE-3/ICE spacecraft, average abundances of He-4, He-3, O, Ne, Si, and Fe have been determined over extended periods. In this paper the abundances of He-4, O, Ne, Si, and Mg obtained by the ICI in the region of sector boundary crossings (SBCs), magnetic clouds and bidirectional streaming events (BDSs) are compared with the average abundances. Both magnetic clouds and BDSs are associated with coronal mass ejections (CMEs). No variation of abundance is seen to occur at SBCs except for helium, as has already been observed. In CME-related material, the abundance of neon appears to be high and variable, in agreement with recent analysis of spectroscopic observations of active regions. We find that our observations can be correlated with the magnetic topology in the corona.
    Keywords: SOLAR PHYSICS
    Type: In: Solar Wind Seven; Proceedings of the 3rd COSPAR Colloquium, Goslar, Germany, Sept. 16-20, 1991 (A93-33554 13-92); p. 379-384.
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  • 2
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    CELIAS: Charge, Element and Isotope Analysis System for the SOHO mission (1992)
    In:  CASI
    Details
    Publication Date: 2006-06-13
    Description: The status and further development as well as first calibration of the CELIAS experiment on SOHO is presented. CELIAS is designed to measure the mass, ionic charge, and energy of low and high speed solar wind of suprathermal ions and of low energy flare particles. Through analysis of the elemental and isotopic abundances (the ionic charge state and velocity distributions of ions originating on the solar atmosphere), the investigation focuses on studying the plasma processes in various temporal and spatial scales in the solar chromosphere, transition zone, and corona. Additionally, the CELIAS experiment includes the Solar EUV Monitor (SEM). This unit, which consists of an EUV transmission grating spectrometer and three isolated silicon photodiodes as detectors, is described. The three mass and charge discriminating sensors based on the time of flight technique are also described.
    Keywords: SOLAR PHYSICS
    Type: ESA, Study of the Solar-Terrestrial System; p 343
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  • 3
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    Space-based measurements of elemental abundances and their relation to solar abundances (1990)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: The Ion Composition Instrument (ICI) aboard the ISEE-3/ICE spacecraft was in the solar wind continuously from August 1978 to December 1982. The results made it possible to establish long-term average solar wind abundance values for helium, oxygen, neon, silicon, and iron. The Charge-Energy-Mass instrument aboard the CCE spacecraft of the AMPTE mission has measured the abundance of these elements in the magnetosheath and has also added carbon, nitrogen, magnesium, and sulfur to the list. There is strong evidence that these magnetosheath abundances are representative of the solar wind. Other sources of solar wind abundances are Solar Energetic Particle experiments and Apollo lunar foils. When comparing the abundances from all of these sources with photospheric abundances, it is clear that helium is depleted in the solar wind while silicon and iron are enhanced. Solar wind abundances for carbon, nitrogen, oxygen, and neon correlate well with the photospheric values. The incorporation of minor ions into the solar wind appears to depend upon both the ionization times for the elements and the Coulomb drag exerted by the outflowing proton flux.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 128; 195-201
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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:  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
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  • 5
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    Helium and minor ions in the corona and solar wind - Dynamics and charge states (1986)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: A theoretical model of the acceleration region of the solar wind with major species (p, alpha, e) and minor ions (e.g., He-3, C, O, Mg, Si) is presented. Observed n(e)-profiles and the equations of continuity and momentum are used to calculate profiles of T, n, and u for all species, as well as charge states of minor ions. The disagreement of the results of a pure p-e model with observations is discussed in some detail, and it is shown that a model consistent with observations both in the corona and at 1 AU requires a finite abundance of He(2+). This model predicts a strong enhancement of He/H in the lower corona. The results for the frozen-in charge states in the p-alpha-e model are in agreement with measurements in the low speed solar wind, especially for the well determined pair O(6+)/O(7+). Finally, a model for a coronal hole is investigated and it is found that wave pressure is necessary to model successfully the observed solar wind speeds and abundances. Although various simplifying assumptions had to be introduced, care was taken to ensure that the model remains physically consistent, i.e., that the same physics is used for the major species as well as the minor ions.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 103; 2, 19; 347-383
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  • 6
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    Determination of solar wind elemental abundances from M/Q observations during three periods in 1980 (1983)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: Mass spectra in the M/Q range from 2 to 3, provided by a high-resolution mode of the ISEE-3 Plasma Composition Experiment, were evaluated for three selected periods during early 1980. The observed Ne/O ratios are compatible with estimated solar abundance ratios. In two of the three periods, the He/Ne-ratios agree with the Apollo foil results. Freezing-in temperatures for oxygen are similar to those obtained by other groups. Possible reasons for an unexpectedly high flux at M/Q = 2.4 are discussed.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 88; 359-376
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  • 7
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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
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  • 8
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    Solar wind iron and oxygen charge states and relative abundances measured by SWICS on Ulysses (1992)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: We present the results of a survey of iron and oxygen charge state distributions as detected by the Solar Wind Ion Composition Spectrometer on the Ulysses spacecraft. The results are categorized in terms of the ionization temperature determined every approximately 13 minute instrument cycle from the O(+7) to O(+6) ratio. Our preliminary Fe/O abundance ratio is 0.12 averaged over this 3 month survey. The Fe charge state distributions accumulated during times of high oxygen ionization temperatures are clearly nonisothermal.
    Keywords: SOLAR PHYSICS
    Type: In: Solar Wind Seven; Proceedings of the 3rd COSPAR Colloquium, Goslar, Germany, Sept. 16-20, 1991 (A93-33554 13-92); p. 369-373.
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  • 9
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    The relative abundance of 3He(++) in the solar wind (1983)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Continuous measurements of solar wind 3He(++) and 4He(++) were made covering a full range of solar wind conditions. The average flux ratio derived from these data is 2310 + or - 50, in excellent agreement with the Apollo foil measurements. A probable correlation between average flux ratio and solar activity was found; however, an examination of the data during periods of 3He(++)-rich solar flares shows no detectable increase in 3He(++) in the solar wind.
    Keywords: SOLAR PHYSICS
    Type: JPL Solar Wind Five; p 591-596
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  • 10
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    Interpretation of 3He variations in the solar wind (1983)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The ion composition instrument (ICI) on ISEE-3 observed the isotopes of helium of mass 3 and 4 in the solar wind almost continuously between August 1978 and July 1982. This period included the increase towards the maximum of solar activity cycle 21, the maximum period, and the beginning of the descent towards solar minimum. Observations were made when the solar wind speed was between 300 and 620 km/s. For part of the period evidence for regular interplanetary magnetic sector structure was clear and a number of 3He flares occurred during this time.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-85049 , NAS 1.15:85049
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