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@Article{HessEcheZark:2012:SoWiPr,
               author = "Hess, S. L. G. and Echer, E. and Zarka, P.",
          affiliation = "LATMOS, IPSL-CNRS, Universit{\'e} Versailles-St Quentin, France 
                         and {Instituto Nacional de Pesquisas Espaciais (INPE)} and LESIA, 
                         Observatoire de Paris, CNRS, Univ. Paris-Diderot, Meudon, France",
                title = "Solar wind pressure effects on Jupiter decametric radio emissions 
                         independent of Io",
              journal = "Planetary and Space Science",
                 year = "2012",
               volume = "70",
               number = "1",
                pages = "114--125",
                month = "Sept.",
             keywords = "Auroral radio emissions, Electrodynamic interaction, 
                         Interplanetary fast shocks, Jovian magnetosphere, Jupiters, 
                         Michigan, Propagation models, Radio data, Radio emission, Solar 
                         wind dynamic pressure, Solar wind interactions, Solar wind 
                         pressure, Ultra-violet, Wind conditions, Decametric radio 
                         emission, Jupiter auroral radio emission, Jupiter magnetosphere, 
                         Solar wind.",
             abstract = "This paper investigates the effects of the solar wind dynamic 
                         pressure on Jupiter auroral radio emissions at decametric 
                         wavelengths that are not controlled by the electrodynamic 
                         interaction with the moon Io (non-Io DAM). In order to conduct 
                         this study, Nanc¸ay decametric array radio data are analyzed for 
                         the 1996-1999 period. Solar wind conditions at Jupiter's orbit are 
                         studied using the Michigan University solar wind propagation model 
                         (mSWiM). Interplanetary fast shocks (forward shocks, FS, or 
                         reverse shocks, RS), and average solar wind dynamic pressure are 
                         correlated with non-Io DAM emission occurrence, duration and 
                         power. It is found that non-Io DAM emissions occur preferentially 
                         during periods of enhanced solar wind dynamic pressure and after a 
                         FS or a RS arrival at Jupiter. The dawn (non-Io B-type) and dusk 
                         (non-Io-A-type) radio emissions are investigated separately and 
                         show (1) a dawn-dusk asymmetry consistent with prior studies and 
                         auroral ultraviolet (UV) observations, and (2) different behaviors 
                         in response to solar wind shocks. Our study confirms the solar 
                         wind control of - at least a part of - the non-Io DAM, and refines 
                         the scenario of response of the radio emissions to the solar wind 
                         interaction with the Jovian magnetosphere.",
                  doi = "{10.1016/j.pss.2012.05.011;}",
                  url = "http://dx.doi.org/{10.1016/j.pss.2012.05.011;}",
                 issn = "0032-0633",
             language = "en",
        urlaccessdate = "28 jan. 2021"
}


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