Ontology type: schema:ScholarlyArticle
2018-09-05
AUTHORSKimberly M. Moore, Rakesh K. Yadav, Laura Kulowski, Hao Cao, Jeremy Bloxham, John E. P. Connerney, Stavros Kotsiaros, John L. Jørgensen, José M. G. Merayo, David J. Stevenson, Scott J. Bolton, Steven M. Levin
ABSTRACTThe Juno spacecraft, which is in a polar orbit around Jupiter, is providing direct measurements of the planet’s magnetic field close to its surface1. A recent analysis of observations of Jupiter’s magnetic field from eight (of the first nine) Juno orbits has provided a spherical-harmonic reference model (JRM09)2 of Jupiter’s magnetic field outside the planet. This model is of particular interest for understanding processes in Jupiter’s magnetosphere, but to study the field within the planet and thus the dynamo mechanism that is responsible for generating Jupiter’s main magnetic field, alternative models are preferred. Here we report maps of the magnetic field at a range of depths within Jupiter. We find that Jupiter’s magnetic field is different from all other known planetary magnetic fields. Within Jupiter, most of the flux emerges from the dynamo region in a narrow band in the northern hemisphere, some of which returns through an intense, isolated flux patch near the equator. Elsewhere, the field is much weaker. The non-dipolar part of the field is confined almost entirely to the northern hemisphere, so there the field is strongly non-dipolar and in the southern hemisphere it is predominantly dipolar. We suggest that Jupiter’s dynamo, unlike Earth’s, does not operate in a thick, homogeneous shell, and we propose that this unexpected field morphology arises from radial variations, possibly including layering, in density or electrical conductivity, or both. More... »
PAGES76-78
http://scigraph.springernature.com/pub.10.1038/s41586-018-0468-5
DOIhttp://dx.doi.org/10.1038/s41586-018-0468-5
DIMENSIONShttps://app.dimensions.ai/details/publication/pub.1106420918
PUBMEDhttps://www.ncbi.nlm.nih.gov/pubmed/30185957
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