Access

You are not currently logged in.

Access your personal account or get JSTOR access through your library or other institution:

login

Log in to your personal account or through your institution.

Energetic Particles in the Jovian Magnetotail

R. L. McNutt Jr., D. K. Haggerty, M. E. Hill, S. M. Krimigis, S. Livi, G. C. Ho, R. S. Gurnee, B. H. Mauk, D. G. Mitchell, E. C. Roelof, D. J. McComas, F. Bagenal, H. A. Elliott, L. E. Brown, M. Kusterer, J. Vandegriff, S. A. Stern, H. A. Weaver, J. R. Spencer and J. M. Moore
Science
New Series, Vol. 318, No. 5848 (Oct. 12, 2007), pp. 220-222
Stable URL: http://www.jstor.org/stable/20048575
Page Count: 3
  • More info
  • Cite this Item
Energetic Particles in the Jovian Magnetotail
Preview not available

Abstract

When the solar wind hits Jupiter's magnetic field, it creates a long magnetotail trailing behind the planet that channels material out of the Jupiter system. The New Horizons spacecraft traversed the length of the jovian magnetotail to >2500 jovian radii ( $R_{\text{J}}$ ; 1 $R_{\text{J}}$ ≡71,400 kilometers), observing a high-temperature, multispecies population of energetic particles. Velocity dispersions, anisotropies, and compositional variation seen in the deep-tail (≥ 500 $R_{\text{J}}$ ) with a ∼3-day periodicity are similar to variations seen closer to Jupiter in Galileo data. The signatures suggest plasma streaming away from the planet and injection sites in the near-tail region (∼200 to 400 $R_{\text{J}}$ ) that could be related to magnetic reconnection events. The tail structure remains coherent at least until it reaches the magnetosheath at 1655 $R_{\text{J}}$ .

Page Thumbnails

  • Thumbnail: Page 
220
    220
  • Thumbnail: Page 
221
    221
  • Thumbnail: Page 
222
    222