Rights statement: This is the author’s version of a work that was accepted for publication in Planetary and Space Science. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Planetary and Space Science, 225, 2022 DOI: 10.1016/j.pss.2022.105609
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Final published version
Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
}
TY - JOUR
T1 - Modelling magnetic fields and plasma flows in the magnetosphere of Jupiter
AU - Millas, D.
AU - Achilleos, N.
AU - Guio, P.
AU - Arridge, C.S.
N1 - This is the author’s version of a work that was accepted for publication in Planetary and Space Science. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Planetary and Space Science, 225, 2022 DOI: 10.1016/j.pss.2022.105609
PY - 2023/1/31
Y1 - 2023/1/31
N2 - The magnetic fields of the giant planets, Jupiter and Saturn, deviate significantly from a pure magnetic dipole and the cold plasma is mostly centrifugally confined near the equator. The additional contribution of the azimuthal currents leads to the stretching of the magnetic field and the formation of a characteristic, disc-type structure known as a magnetodisc. We present here an updated version of a numerical implementation of Caudal's iterative scheme, used to create models of the magnetosphere. In particular, we include newer equatorial density, temperature and hot plasma profiles obtained from Galileo data. Finally, we describe and use an algorithm to update the angular velocity profile after the end of the iterative process, using information from the magnetodisc. We also present comparisons between the azimuthal current and plasma flow predicted by our model and those derived from spacecraft observations.
AB - The magnetic fields of the giant planets, Jupiter and Saturn, deviate significantly from a pure magnetic dipole and the cold plasma is mostly centrifugally confined near the equator. The additional contribution of the azimuthal currents leads to the stretching of the magnetic field and the formation of a characteristic, disc-type structure known as a magnetodisc. We present here an updated version of a numerical implementation of Caudal's iterative scheme, used to create models of the magnetosphere. In particular, we include newer equatorial density, temperature and hot plasma profiles obtained from Galileo data. Finally, we describe and use an algorithm to update the angular velocity profile after the end of the iterative process, using information from the magnetodisc. We also present comparisons between the azimuthal current and plasma flow predicted by our model and those derived from spacecraft observations.
KW - Angular velocity
KW - Magnetohydrodynamics (MHD)
KW - Numerical methods
KW - Planetary magnetic fields
KW - Iterative methods
KW - Magnetohydrodynamics
KW - Magnetoplasma
KW - Planets
KW - Plasma devices
KW - Plasma flow
KW - Plasma jets
KW - Azimuthal current
KW - Cold plasmas
KW - Current leads
KW - Disk-type
KW - Giant planets
KW - Jupiters
KW - Magnetic plasma
KW - Magnetic-field
KW - Magnetohydrodynamic
U2 - 10.1016/j.pss.2022.105609
DO - 10.1016/j.pss.2022.105609
M3 - Journal article
VL - 225
JO - Planetary and Space Science
JF - Planetary and Space Science
SN - 0032-0633
M1 - 105609
ER -