@InProceedings{RodríguezGómesEcheMagaMarq:2018:StSoWi,
               author = "Rodr{\'{\i}}guez G{\'o}mes, Jenny Marcela and Echer, Ezequiel 
                         and Magalh{\~a}es, Fab{\'{\i}}ola Pinho and Marques, M.",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)} and {Universidade Federal do Rio 
                         Grande do Norte (UFRN)}",
                title = "A study of solar wind effects of Jupiter magnetosphere",
                 year = "2018",
         organization = "Simp{\'o}sio Brasileiro de Geof{\'{\i}}sica Espacial e 
                         Aeronomia, 7. (SBGEA)",
             abstract = "The Sun drives many phenomena in the solar system. Its influence 
                         is mainly due to the magnetic phenomena. The solar wind 
                         interaction with the bodies of the solar system results in the 
                         formation of the magnetospheres. The Jupiter's magnetosphere in 
                         part is sensitive to the solar wind dynamic pressure variations. 
                         Several observations shown that aurora and radio emissions are 
                         intensified during higher solar wind pressure or induced by 
                         interplanetary shocks. Interplanetary shocks are driven by ICMEs 
                         or CIRS. The fast forward (FS) shock is mainly by ICMEs originated 
                         from CMEs. However, when CHs are evolving, fast streams emanate, 
                         and intercept the ambient solar wind. This interaction forms a 
                         compression region between the high speed stream and slow speed 
                         stream, it is limited by fast forward (FS) and fast reverse (RS) 
                         shocks. We present a study of fast forward and reverse shocks on 
                         the Jupiter magnetosphere. For this purpose, we use the propagated 
                         solar wind from Michigan Solar Wind model (mSWim) during the 
                         outbound period of the Cassini spacecraft. Also, the dynamic 
                         pressure will be obtained and analyzed. This work can contribute 
                         to understanding the complex Jupiter magnetosphere and its 
                         interaction with the solar wind.",
  conference-location = "Santa Maria, RS",
      conference-year = "05-09 nov",
             language = "pt",
        urlaccessdate = "28 abr. 2024"
}