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  • Heliosphere  (3)
  • LUNAR AND PLANETARY EXPLORATION  (1)
  • PHYSICS, ATOMIC, MOLECULAR, AND NUCLEAR  (1)
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  • 1
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    Unknown
    Energetic particle storage on the sun (1973)
    In:  CASI
    Details
    Publication Date: 2006-04-05
    Description: The storage of energetic electron and protons of energies much greater than 1 GeV in the solar corona is investigated.
    Keywords: PHYSICS, ATOMIC, MOLECULAR, AND NUCLEAR
    Type: NASA, Washington High Energy Phenomena on the Sun; p 503-515
    Format: text
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    NASA TECHNICAL REPORTS
  • 2
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    The hot plasma environment at Jupiter - Ulysses results (1992)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: Initial results obtained from measurements made by the HI-SCALE (heliosphere instrument for spectra, composition, and anisotropy at low energies) experiment are reported. Data revealed that the Jovian magnetosphere is very extended, with the day-side magnetopause located at about 105 Jupiter radii. The relative abundances of sulfur, oxygen, and sodium to helium decreased with the decreasing radial distance from the planet on the day-side, which suggests that the abundances of Jupiter-derived species are dependent on latitude. Intense fluxes of counter-streaming ions and electrons were discovered in the dusk-side, high-latitude region from the edge of the plasma sheet to the dusk-side magnetopause. These beams of ions and electrons appeared to be very tightly aligned with the magnetic field and to be superimposed on a time- and space variable isotropic hot plasma background. The current carried by measured hot plasma particles are about 1.6 x 10 exp -4 microamps per sq m.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science (ISSN 0036-8075); 257; 5076; 1518-152
    Format: text
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    NASA TECHNICAL REPORTS
  • 3
    Electronic Resource
    Electronic Resource
    Co-rotating particle enhancements out of the ecliptic plane (1995)
    Springer
    Space science reviews 72 (1995), S. 327-330 
    Details
    ISSN: 1572-9672
    Keywords: Heliosphere ; Energetic particles ; co-rotating interaction regions
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The characteristics of the recurrent electron (38–53 keV) and ion (〉∼0.5 MeV) enhancements observed by Ulysses from mid-1992 to April 1994 are presented. The magnitude of the ion flux increases reached a maximum at a latitude of ∼20°S and decreased afterwards by ∼23%/degree until early 1994. The magnitude of the electron increases showed a similar trend until May, 1993, after which time it became approximately constant, until it started to increase again in early 1994. The electron enhancements have lagged the protons by up to 5 days once Ulysses left the heliospheric current sheet (mid-1993). The electron spectral index tended to harden (a) during the decay of the event and (b) as the latitude increased, up to 50°S. The events have recurred on a 26.0 day period, but with significant phase shifts over the 25 rotations studied. The H/He ratio decreases across the maximum intensity. The mean minimum value for H/He was 3.5±0.3, lower than that measured in previous studies in the ecliptic plane.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00768799
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    Paper (German National Licenses)
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  • 4
    Electronic Resource
    Electronic Resource
    IMF connection for energetic protons observed at Ulysses via mid-latitude solar wind rarefaction regions (1995)
    Springer
    Space science reviews 72 (1995), S. 309-314 
    Details
    ISSN: 1572-9672
    Keywords: Heliosphere ; Energetic particles ; Corotating high-speed streams
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract As Ulysses moved inward and southward from mid-1992 to early 1994 we noticed the occasional occurrence of “inter-events”, lasting about 10 days and falling between the recurrent events, observed at proton energies of 0.48–97 MeV, associated with Corotating Interaction Regions (CIR). These inter-events were present for several sequences of two or more solar rotations at intensity levels around 1% of those of the neighbouring main events. When we compared the Ulysses events with those measured on IMP-8 at 1 AU we saw that the inter-events appeared at Ulysses after the extended emission (〉10 days) of large fluxes of solar protons of the same energy that lasted at least one solar rotation at 1 AU. The inter-events fell completely within the rarefaction regions (dv/dt〈0) of the recurrent solar wind streams. The interplanetary magnetic field (IMF) lines in the rarefactions map back to the narrow range of longitudes at the Sun which mark the eastern edge of the source region of the high speed stream. Thus the inter-events are propagating at mid-latitudes to Ulysses along field lines free from stream-stream interactions. They are seen in the 0.39–1.28 MeV/nucleon He, which exhibit a faster decay, but almost never in the 38–53 keV electrons. We show that the inter-events are unlikely to be accelerated by reverse shocks associated with the CIRs and that they are more likely to be accelerated by sequences of solar events and transported along the IMF in the rarefactions of the solar wind streams.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00768796
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  • 5
    Electronic Resource
    Electronic Resource
    Reverse shock acceleration of electrons and protons at mid-heliolatitudes from 5.3-3.8 AU (1995)
    Springer
    Space science reviews 72 (1995), S. 303-308 
    Details
    ISSN: 1572-9672
    Keywords: Heliosphere ; Energetic particles ; Shock acceleration ; Reverse shocks
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We examine the intensity, anisotropy and energy spectrum of 480–966 keV protons and 38–315 keV electrons observed by the HI-SCALE instrument on Ulysses associated with Corotating Interaction Regions (CIR) from mid-1992 to early 1994. The particle events are most clearly ordered by the reverse shocks bounding the CIRs. The bulk of the ion fluxes appear either straddling, or with their maximum intensity following, the reverse shock. The electron intensities rise sharply to their maximum upon the passage of the reverse shock, and are delayed with respect to the protons. We believe that following acceleration at the reverse shock the electrons re-enter the inner heliosphere and mirror, to return to the reverse shock for repeated acceleration. This process is more effective for electrons (v∼c/2) than for ions, and also favours the higher velocity electrons, which accounts for the observed spectral hardening with latitude.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00768795
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    Paper (German National Licenses)
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