Structure of the Jovian magnetodisk current sheet:: initial Galileo observations |
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| Institution: | 1. Institute of Geophysics and Planetary Physics, 3845 Slichter Hall, University of California, Los Angeles 90095-1567, USA;1. Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Université Paris Diderot, UMR 7154 CNRS, F-75005 Paris, France;2. Institute of Physics of the Earth, Russian Academy of Sciences, Moscow, Russia;3. State Historical Museum, Moscow, Russia;4. Plateforme Rayons X, UFR de Chimie, Université Paris Diderot, F-75013 Paris, France;1. Universidade Estadual da Paraiba, Campina Grande, PB, Brazil;2. Instituto Nacional de Pesquisas Espaciais, Sao Jose dos Campos, SP, Brazil;3. Universidade Federal de Campina Grande, Campina Grande, PB, Brazil;4. Centro Regional Sul de Ciencias Espaciais, Santa Maria, RS, Brazil;1. Navigation Instrument Research Institute, Harbin Institute of Technology, Harbin, Heilongjiang, China;2. College of Automation, Harbin Engineering University, Harbin, Heilongjiang, China;1. Southwest Research Institute, Space Science and Engineering, TX, United States;2. Finnish Meteorological Institute, Finland;3. University of Virginia, VA, United States |
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| Abstract: | The ten-degree tilt of the Jovian magnetic dipole causes the magnetic equator to move back and forth across Jupiters rotational equator and the Galileo orbit that lies therein. Beyond about 24 Jovian radii, the equatorial current sheet thins and the magnetic structure changes from quasi-dipolar into magnetodisk-like with two regions of nearly radial but antiparallel magnetic field separated by a strong current layer. The magnetic field at the center of the current sheet is very weak in this region. Herein we examine the current sheet at radial distances from 24–55 Jovian radii. We find that the magnetic structure very much resembles the structure seen at planetary magnetopause and tail current sheet crossings. The magnetic field variation is mainly linear with little rotation of the field direction. At times there is almost no small-scale structure present and the normal component of the magnetic field is almost constant through the current sheet. At other times there are strong small-scale structures present in both the southward and northward directions. This small-scale structure appears to grow with radial distance and may provide the seeds for the explosive reconnection observed at even greater radial distances on the nightside. Beyond about 40 Jovian radii, the thin current sheet also appears to be almost constantly in oscillatory motion with periods of about 10 min. The amplitude of these oscillations also appears to grow with radial distance. The source of these fluctuations may be dynamical events in the more distant magnetodisk. |
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