scholarly journals Galileo observes electromagnetically coupled dust in the Jovian magnetosphere

1998 ◽  
Vol 103 (E9) ◽  
pp. 20011-20022 ◽  
Author(s):  
E. Grün ◽  
H. Krüger ◽  
A. L. Graps ◽  
D. P. Hamilton ◽  
A. Heck ◽  
...  
Keyword(s):  
Jovian Magnetosphere

scholarly journals The composition of Europa's near-surface atmosphere

2008 ◽  
Vol 4 (S251) ◽  
pp. 327-328
Author(s):  
Mau C. Wong ◽  
Tim Cassidy ◽  
Robert E. Johnson
Keyword(s):  
Solar System ◽  
Surface Composition ◽  
Near Surface ◽  
Water Ice ◽  
Model Studies ◽  
Surface Atmosphere ◽  
Jovian Magnetosphere ◽  
Ice Surface ◽  
Geophysical Phenomenon ◽  
Inorganic Species

AbstractThe presence of an undersurface ocean renders Europa as one of the few planetary bodies in our Solar System that has been conjectured to have possibly harbored life. Some of the organic and inorganic species present in the ocean underneath are expected to transport upwards through the relatively thin ice crust and manifest themselves as impurities of the water ice surface. For this reason, together with its unique dynamic atmosphere and geological features, Europa has attracted strong scientific interests in past decades.Europa is imbedded inside the Jovian magnetosphere, and, therefore, is constantly subjected to the immerse surrounding radiations, similar to the other three Galilean satellites. The magnetosphere-atmosphere-surface interactions form a complex system that provides a multitude of interesting geophysical phenomenon that is unique in the Solar System. The atmosphere of Europa is thought to have created by, mostly, charged particles sputtering of surface materials. Consequently, the study of Europa's atmosphere can be used as a tool to infer the surface composition. In this paper, we will discuss our recent model studies of Europa's near-surface atmosphere. In particular, the abundances and distributions of the dominant O2 and H2O species, and of other organic and inorganic minor species will be addressed.

Evidence for chaotic dynamics in the Jovian magnetosphere

2004 ◽  
Vol 52 (5-6) ◽  
pp. 513-541 ◽  
Author(s):  
G.P. Pavlos ◽  
M.A. Athanasiu ◽  
G.C. Anagnostopoulos ◽  
A.G. Rigas ◽  
E.T. Sarris
Keyword(s):  
Chaotic Dynamics ◽  
Jovian Magnetosphere

Ion measurements in the Jovian magnetosphere by the Ulysses EPAC experiment: A comparison between dawn and dusk sectors

1995 ◽  
Vol 16 (4) ◽  
pp. 183-186 ◽  
Author(s):  
N. Krupp ◽  
E. Keppler ◽  
A. Korth ◽  
M. Fränz ◽  
M.K. Reuss ◽  
...  
Keyword(s):  
Jovian Magnetosphere

An analytical model of the Jovian magnetosphere

1975 ◽  
Vol 2 (7) ◽  
pp. 269-272 ◽  
Author(s):  
Franklin D. Barish ◽  
Robert A. Smith
Keyword(s):  
Analytical Model ◽  
Jovian Magnetosphere

scholarly journals A summary of observational records on periodicities above the rotational period in the Jovian magnetosphere

2009 ◽  
Vol 27 (6) ◽  
pp. 2565-2573 ◽  
Author(s):  
E. A. Kronberg ◽  
J. Woch ◽  
N. Krupp ◽  
A. Lagg
Keyword(s):  
Data Sets ◽  
Mass Loading ◽  
Triggering Mechanism ◽  
Release Process ◽  
Jovian Magnetosphere ◽  
Planetary Rotation ◽  
Mass Release ◽  
Two Phases ◽  
Associated Mass

Abstract. The Jovian magnetosphere is a very dynamic system. The plasma mass-loading from the moon Io and the fast planetary rotation lead to regular release of mass from the Jovian magnetosphere and to a change of the magnetic topology. These regular variations, most commonly on several (2.5–4) days scale, were derived from various data sets obtained by different spacecraft missions and instruments ranging from auroral images to in situ measurements of magnetospheric particles. Specifically, ion measurements from the Galileo spacecraft represent the periodicities, very distinctively, namely the periodic thinning of the plasma sheet and subsequent dipolarization, and explosive mass release occurring mainly during the transition between these two phases. We present a review of these periodicities, particularly concentrating on those observed in energetic particle data. The most distinct periodicities are observed for ions of sulfur and oxygen. The periodic topological change of the Jovian magnetosphere, the associated mass-release process and auroral signatures can be interpreted as a global magnetospheric instability with analogies to the two step concept of terrestrial substorms. Different views on the triggering mechanism of this magnetospheric instability are discussed.

A Cyclotron Theory for the Beaming Pattern of Jupiter’s Decametric Radio Emission

1981 ◽  
Vol 4 (2) ◽  
pp. 221-226 ◽  
Author(s):  
R. G. Hewitt ◽  
D. B. Melrose ◽  
K. G. Rönnmark
Keyword(s):  
Magnetic Field ◽  
Radio Emission ◽  
Observational Data ◽  
Theoretical Interpretation ◽  
Theoretical Interest ◽  
Hollow Cone ◽  
The Past ◽  
Jovian Magnetosphere ◽  
Half Angle ◽  
Occurrence Pattern

Ground-based observations of Jupiter’s decametric radio emission (DAM) have been reviewed by Ellis (1965), Warwick (1967, 1970) and Carr and Gulkis (1969). A startling feature of DAM is the modulating effect of Io, and interpretation of the Io effect has dominated theoretical discussions of DAM until quite recently, specifically until the fly-by s of Voyagers 1 and 2. The Voyager data showed that the DAM appears as nested arcs in the frequency-Jovian longitude plane (Warwick et al. 1979, Boischot et al. 1981). The interpretation of this arc structure has been of primary theoretical interest over the past two years. The most widely adopted explanation is that the emission from each point is confined to the surface of a hollow cone (Goldstein and Thieman 1981). This idea is not new: emission on the surface of a cone was discussed by Ellis and McCulloch (1963); Dulk (1967) derived detailed parameters for the cone (half angle 79° width 1°) from the occurrence pattern of DAM; and Goldreich and Lynden-Bell (1969) presented a theoretical interpretation of it. More recently Goldstein et al. (1979) used observational data on the Jovian magnetic field in deriving properties of the required emission cone. It seems that one requires the properties of the emission cone to vary with position in the Jovian magnetosphere to account for the nested arc pattern (Goldstein and Thieman 1981; Gurnett and Goertz 1981).

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