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Io‐Jupiter decametric arcs observed by Juno/Waves compared to ExPRES simulations
Author(s) -
Louis C. K.,
Lamy L.,
Zarka P.,
Cecconi B.,
Imai M.,
Kurth W. S.,
Hospodarsky G.,
Hess S. L. G.,
Bonnin X.,
Bolton S.,
Connerney J. E. P.,
Levin S. M.
Publication year - 2017
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1002/2017gl073036
Subject(s) - physics , jupiter (rocket family) , maser , cyclotron , astrophysics , latitude , galilean moons , radio wave , southern hemisphere , geophysics , computational physics , plasma , atmospheric sciences , astronomy , planet , spacecraft , nuclear physics , quantum mechanics , natural satellite
We compare observations from the Juno/Waves radio experiment with simulations of radio «arcs» in the time‐frequency plane resulting from the Io‐Jupiter interaction, performed with the ExPRES code. We identify the hemisphere of origin of the observed arcs directly from simulations and confirm this identification through comparison with Juno, Nançay, and Wind observations. The occurrence and shape of observed arcs are well modeled, at low latitudes with their usual shapes as seen from Earth, as well as at high latitudes with longer, bowl‐shaped, arcs observed for the first time. Predicted emission is actually observed only when the radio beaming angle θ = ( k , B ) ≥ 70° ± 5°, providing new constraints on the generation of the decameter emission by the Cyclotron Maser Instability. Further improvements of ExPRES are outlined, which will then be applied to Juno and Earth‐based observations of radio emissions induced by other Galilean satellites or associated to the main auroral oval.