| Texto completo | |
| Autor(es): |
Zarka, P.
[1, 2]
;
Magalhaes, F. P.
[1]
;
Marques, M. S.
[3]
;
Louis, C. K.
[4, 5]
;
Echer, E.
[6]
;
Lamy, L.
[1, 2]
;
Cecconi, B.
[1, 2]
;
Prange, R.
[1]
Número total de Autores: 8
|
| Afiliação do(s) autor(es): | [1] Univ Paris, Observ Paris, LESIA, CNRS, PSL, Sorbonne Univ, Meudon - France
[2] Univ Orleans, Stn Radioastron Nancay, USN, Observ Paris, CNRS, PSL, Nancay - France
[3] Univ Fed Rio Grande do Norte, Dept Geofs, Natal, RN - Brazil
[4] Dublin Inst Adv Studies, Sch Cosm Phys, DIAS Dunsink Observ, Dublin - Ireland
[5] Univ Toulouse, Inst Rech Astrophys & Planetol IRAP, CNRS, CNES, UPS, Toulouse - France
[6] Inst Nacl Pesquisas Espaciais INPE, Sao Jose Dos Campos - Brazil
Número total de Afiliações: 6
|
| Tipo de documento: | Artigo Científico |
| Fonte: | JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS; v. 126, n. 10 OCT 2021. |
| Citações Web of Science: | 0 |
| Resumo | |
Reanalyzing Cassini radio observations performed during Jupiter's flyby of 2000-2001, we study the internal (rotational) versus external (solar wind) control of Jupiter's radio emissions, from kilometer to decameter wavelengths, and the relations between the different auroral radio components. For that purpose, we build a database of the occurrence of Jovian auroral radio components bKOM, HOM, and DAM observed by Cassini, and then frequency-longitude stacked plots of the polarized intensity of these radio components. Comparing the results obtained inbound and outbound, as a function of the Observer's or Sun's longitude, we find that HOM \& DAM are dominantly rotation-modulated (i.e., emitted from searchlight-like sources fixed in Jovian longitude), whereas bKOM is modulated more strongly by the solar wind than by the rotation (i.e., emitted from sources more active within a given Local Time sector). We propose a simple analytical description of these internal and external modulations and evaluate its main parameters (the amplitude of each control) for HOM + DAM and bKOM. Comparing Cassini and Nancay Decameter Array data, we find that HOM is primarily connected to the decameter emissions originating from the dusk sector of the Jovian magnetosphere. HOM and DAM components form a complex but stable pattern in the frequency-longitude plane. HOM also seems to be related to the ``lesser arcs{''} identified by Voyager. bKOM consists of a main part above similar to 40 kHz in antiphase with HOM occurrence, and detached patches below similar to 80 kHz in phase with HOM. The frequency-longitude patterns formed by DAM, HOM and bKOM remain to be modeled. (AU) | |
| Processo FAPESP: | 18/21657-1 - Estudo da variabilidade da atividade auroral em rádio da magnetosfera de Júpiter |
| Beneficiário: | Ezequiel Echer |
| Modalidade de apoio: | Auxílio à Pesquisa - Regular |