Hot plasma and energetic particles in Neptune's magnetosphere

Journal Article · Thu Dec 14 23:00:00 EST 1989 · Science (Washington, D.C.); (United States)

DOI:https://doi.org/10.1126/science.246.4936.1483· OSTI ID:5452626

Krimigis, S M; Bostrom, C O; Cheng, A G; Keath, E P; Mauk, B H ^[1]; Armstrong, T P ^[2]; Axford, W I ^[3]; Gloeckler, G; Hamilton, D C ^[4]; Lanzerotti, L J ^[5]; Van Allen, J A ^[6]

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1. Johns Hopkins Univ., Laurel, MD (USA)
2. Univ. of Kansas, Lawrence (USA)
3. Max-Planck-Institut fuer Aeronomie, Lindau (West Germany)
4. Univ. of Maryland, College Park (USA)
5. AT T Bell Laboratories, Murray Hill, NJ (USA)
6. Univ. of Iowa, Iowa City (USA)

The low-energy charged particle (LECP) instrument on Voyager 2 measured within the magnetosphere of Neptune energetic electrons (22 kiloelectron volts {le} E {le} 20 megaelectron volts) and ions (28 keV {le} E {le} 150 MeV) in several energy channels, including compositional information at higher ({approx lt}0.5 MeV per nucleon) energies, using an array of solid-state detectors in various configurations. The results obtained so far may be summarized as follows: (i) A variety of intensity, spectral, and anisotropy features suggest that the satellite Triton is important in controlling the outer regions of the Neptunian magnetosphere. (ii) Intensities decrease sharply at all energies near the time of closest approach, the decreases being most extended in time at the highest energies, reminiscent of a spacecraft's traversal of Earth's polar regions at low altitudes; simultaneously, several spikes of spectrally soft electrons and protons were seen (power input {approx} 5 x 10{sup {minus}4} ergs cm{sup {minus}2} s{sup {minus}1}) suggestive of auroral processes at Neptune. (iii) Composition measurements revealed the presence of H, H{sub 2}, and He{sup 4}, with relative abundances of 1300:1:0.1, suggesting a Neptunian ionospheric source for the trapped particle population. (iv) Plasma pressures at E {approx lt} 28 keV are maximum at the magnetic equator with {beta} {approx} 0.2, suggestive of a relatively empty magnetosphere, similar to that of Uranus. (v) A potential signature of satellite 1989N1 was seen, both inbound and outbound; other possible signatures of the moons and rings are evident in the data but cannot be positively identified in the absence of an accurate magnetic-field model close to the planet.

• OSTI ID: 5452626
• Journal Information: Science (Washington, D.C.); (United States), Journal Name: Science (Washington, D.C.); (United States) Vol. 246:4936; ISSN SCIEA; ISSN 0036-8075
• Country of Publication: United States
• Language: English

Related Subjects

640107* -- Astrophysics & Cosmology-- Planetary Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
AURORAE
CHARGED PARTICLES
CHARGED-PARTICLE PRECIPITATION
COMPARATIVE EVALUATIONS
ELECTRON DENSITY
ELECTRON PRECIPITATION
EVALUATION
HOT PLASMA
ION DENSITY
IONIC COMPOSITION
NEPTUNE PLANET
PLANETARY ATMOSPHERES
PLANETARY MAGNETOSPHERES
PLANETS
PLASMA
SATELLITES
SURFACES