The low energy plasma in the Jovian magnetosphere

Belcher, J. W.; Goertz, C. K.; Bridge, H. S.

doi:10.1029/gl007i001p00017

Cited by 118 publications

(96 citation statements)

References 9 publications

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“…Actually, the data obtained through in situ observations by spacecraft indicated the remarkable features which suggest rotational effects. For example, the Jovian magnetosphere has a thin disc-like region in which a dense plasma is confined [Belcher, 1983]. Furthermore, the observation that the location of the day side boundary is highly time variable suggests that the structure of the Jovian magnetopause may be much sensitive to the physical parameters of the solar wind [Acu•a et al, 1983].…”

Section: Introductionmentioning

confidence: 99%

MHD simulation of a rapidly rotating magnetosphere interacting with the external plasma flow

Miyoshi

Kusano

1997

Geophysical Research Letters

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Abstract.The nonlinear interaction of a rapidly rotating magnetosphere with the external supersonic plasma flow is investigated by using the three-dimensional global magnetohydrodynamic (MHD) simulation. The results of the simulations clearly indicate that various dawn-dusk asymmetries are generated due to the effect of the rotation. Particularly, the location of the plasmoid, which is generated in the tail region of the rotating magnetosphere, is quite different from the case without rotation.It is also found that distinctive magnetospheric structures such as the plasma disc are largely modified in response to the dynamic pressure in the external plasma flow.ture is still unclear even qualitatively. In this study, we investigate in detail the nonlinear interaction of a rapidly rotating magnetosphere with the external supersonic plasma flow using the three-dimensional global MHD simulations, and theoretically reveal the global structure in the middle and the outer magnetosphere of Jupiter. Simulation ModelAs the basic equations, we adopt the following form of the MHD equations in those the potential field B0 is excluded from the variables [Tanaka, 1994[Tanaka, , 1995'

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Section: Introductionmentioning

confidence: 99%

MHD simulation of a rapidly rotating magnetosphere interacting with the external plasma flow

Miyoshi

Kusano

1997

Geophysical Research Letters

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“…One of the most important influences on the Jovian magnetosphere is the satellite Io (orbiting at-5.9 Rj) with its volcanic plumes and partial atmosphere. The Io-generated gases populate a dense plasma toms near Io's orbit and provide a strong source of hot and cold plasmas throughout the Jovian magnetosphere [Belcher, 1983;Krimigis and Roelof, 1983]. Temporal events can happen in association with the processes that transport the dense iogenic plasmas away from Io.…”

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confidence: 99%

Storm‐like dynamics of Jupiter's inner and middle magnetosphere

Mauk¹,

Williams²,

McEntire³

et al. 1999

J. Geophys. Res.

111

168

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Abstract. The discovery of energy-time dispersed, charged particle signatures of dynamic, longitudinally confined charged particle injections within Jupiter's inner magnetosphere has been reported previously as measured in >20-keV particle intensities by the Galileo energetic particles detector (EPD). While these events have similarities to so-called substorm injections observed within the Earth's magnetosphere, it is unknown whether the driving mechanisms are similar. Over 100 Jovian injection events have now been documented between radial distances of -9 Rj (the inner boundary of most of the observations) and 27 Rj. Injections occur at all System III longitudes and local time positions. Similar to Earth magnetospheric injections, the Jovian injections occur throughout the broad radial region of transition between the quasidipolar and neutral sheet magnetic field configurations, and where the charged particle energy densities are competitive with the magnetic energy densities. The Jovian injections can be clustered in time, analogous to what often happens during well-known magnetic storms that occur in the Earth's magnetosphere. During one particular periapsis of Galileo's orbital trajectory, the magnetosphere was observed by EPD to become suddenly very disturbed with multiple injections following a prolonged period (>24 Earth hours) of relative quiescence. Because of the prestorm coincidence of a signature of an apparent Earth-like global magnetospheric disturbance, we hypothesize that this Jovian storm occurred when the inner and middle magnetosphere were triggered out of marginal stability by the passage of a magnetohydrodynamic fast mode wave launched at the magnetopause by a pressure variation in the interplanetary (solar wind) environment.

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“…As the magnetic dipole of Jupiter is tilted by 10 • with respect to its rotation axis, the material left in the plasma forms a precessing torus, the Io plasma torus. Its ion composition is dominated by the volcanic material erupting at Io's surface (Belcher, 1983). Io's atmosphere and surface-atmosphere interactions are reviewed by Lellouch (2005) in this volume.…”

Section: Interaction Of Io With the Jovian Magnetospherementioning

confidence: 99%

Solar System Magnetospheres

2005

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This article proposes a short review of our present knowledge of solar system magnetospheres, with the purpose of placing the study of Saturn's magnetosphere in the context of a comparative approach. We describe the diversity of solar system magnetospheres and the underlying causes of this diversity: nature and magnetization state of the planetary obstacle, presence or not of a dense atmosphere, rotation state of the planet, existence of a system of satellites, rings and neutral gas populations in orbit around the planet. We follow the "russian doll" hierarchy of solar system magnetospheres to briefly describe the different objects of this family: the heliosphere, which is the Sun's magnetosphere; the "elementary" magnetospheres of the inner planets, Earth and Mercury; the "complex" magnetospheres of the giant planets, dominated by planetary rotation and the presence of interacting objects within their magnetospheric cavities, some of which, like Ganymede, Io or Titan, produce small intrinsic or induced magnetospheres inside the large one. We finally describe the main original features of Saturn's magnetosphere as we see them after the Voyager fly-bys and before the arrival of Cassini at Saturn, and list some of the key questions which Cassini will have to address during its four-year orbital tour.

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The low energy plasma in the Jovian magnetosphere

Cited by 118 publications

References 9 publications

MHD simulation of a rapidly rotating magnetosphere interacting with the external plasma flow

MHD simulation of a rapidly rotating magnetosphere interacting with the external plasma flow

Storm‐like dynamics of Jupiter's inner and middle magnetosphere

Solar System Magnetospheres

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