Juno Mission; Jupiter dynamo; Jupiter interior; Jupiter planetary magnetic field; magnetic field generation; secular variation; Geophysics; Geochemistry and Petrology; Earth and Planetary Sciences (miscellaneous); Space and Planetary Science
Abstract :
[en] A spherical harmonic model of the magnetic field of Jupiter is obtained from vector magnetic field observations acquired by the Juno spacecraft during 32 of its first 33 polar orbits. These Prime Mission orbits sample Jupiter's magnetic field nearly uniformly in longitude (∼11° separation) as measured at equator crossing. The planetary magnetic field is represented with a degree 30 spherical harmonic and the external field is approximated near the origin with a simple external spherical harmonic of degree 1. Partial solution of the underdetermined inverse problem using generalized inverse techniques yields a model (“JRM33”) of the planetary magnetic field with spherical harmonic coefficients reasonably well determined through degree and order 13. Useful information regarding the field extends through degree 18, well fit by a Lowes' spectrum with a dynamo core radius of 0.81 Rj, presumably the outer radius of the convective metallic hydrogen region. This new model provides a most detailed view of a planetary dynamo and evidence of advection of the magnetic field by deep zonal winds in the vicinity of the Great Blue Spot (GBS), an isolated and intense patch of flux near Jupiter's equator. Comparison of the JRM33 and JRM09 models suggests secular variation of the field in the vicinity of the GBS during Juno's nearly 5 years of operation in orbit about Jupiter. The observed secular variation is consistent with the penetration of zonal winds to a depth of ∼3,500 km where a flow velocity of ∼0.04 ms−1 is required to match the observations.
Research Center/Unit :
STAR - Space sciences, Technologies and Astrophysics Research - ULiège
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Connerney, J.E.P. ; Space Research Corporation, Annapolis, United States ; NASA Goddard Space Flight Center, Greenbelt, United States
Timmins, S.; NASA Goddard Space Flight Center, Greenbelt, United States ; ADNET Systems, Inc., Bethesda, United States
Oliversen, R.J. ; NASA Goddard Space Flight Center, Greenbelt, United States
Espley, J.R. ; NASA Goddard Space Flight Center, Greenbelt, United States
Joergensen, J.L.; Technical University of Denmark (DTU), Kongens Lyngby, Denmark
Kotsiaros, S. ; Technical University of Denmark (DTU), Kongens Lyngby, Denmark
Joergensen, P.S. ; Technical University of Denmark (DTU), Kongens Lyngby, Denmark
Merayo, J.M.G. ; Technical University of Denmark (DTU), Kongens Lyngby, Denmark
Herceg, M. ; Technical University of Denmark (DTU), Kongens Lyngby, Denmark
Bloxham, J. ; Harvard University, Cambridge, United States
Moore, K.M. ; California Institute of Technology, Pasadena, United States
Mura, A. ; INAF-IAPS, Rome, Italy
Moirano, Alessandro ; Université de Liège - ULiège > Département d'astrophysique, géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP) ; INAF-IAPS, Rome, Italy
Bolton, S.J. ; Southwest Research Institute, San Antonio, United States
Levin, S.M. ; California Institute of Technology, Pasadena, United States ; Jet Propulsion Laboratory (JPL), Pasadena, United States
We thank the project and support staff at the Jet Propulsion Laboratory (JPL), Lockheed Martin, and the Southwest Research Institute (SWRI) for the design, implementation, and operation of the Juno spacecraft. The Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration (80NM0018D0004), manages the Juno mission for the principal Investigator, S. Bolton, of SWRI. We especially thank Monte Kaelberer, Ever Guandique, and Paul Romani at GSFC and Carol Ladd at the Space Research Corporation for expert support. K. Moore acknowledges financial support via the 51 Pegasi b Fellowship from the the Heising-Simons Foundation. This research is supported by the Juno Project under NASA grant NNM06AAa75c to SWRI, and NASA grant NNN12AA01C to JPL/Caltech. The Juno mission is part of the New Frontiers Program managed at NASA's Marshall Space Flight Center in Huntsville, Alabama.We thank the project and support staff at the Jet Propulsion Laboratory (JPL), Lockheed Martin, and the Southwest Research Institute (SWRI) for the design, implementation, and operation of the Juno spacecraft. The Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration (80NM0018D0004), manages the Juno mission for the principal Investigator, S. Bolton, of SWRI. We especially thank Monte Kaelberer, Ever Guandique, and Paul Romani at GSFC and Carol Ladd at the Space Research Corporation for expert support. K. Moore acknowledges financial support via the 51 Pegasi b Fellowship from the the Heising‐Simons Foundation. This research is supported by the Juno Project under NASA grant NNM06AAa75c to SWRI, and NASA grant NNN12AA01C to JPL/Caltech. The Juno mission is part of the New Frontiers Program managed at NASA's Marshall Space Flight Center in Huntsville, Alabama.
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