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@Article{RodríguezGómezPalaVieiLago:2019:PlEvTh,
               author = "Rodr{\'{\i}}guez G{\'o}mez, Jenny Marcela and Palacios, Judith 
                         and Vieira, Luis Eduardo Antunes and Lago, Alisson Dal",
          affiliation = "{Skolkovo Institute of Science and Technology} and {Leibniz 
                         Institut f{\"u}r Sonnenphysik (KIS)} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)} and {Instituto Nacional de Pesquisas 
                         Espaciais (INPE)}",
                title = "The plasma B evolution through the solar corona during solar 
                         cycles 23 and 24",
              journal = "The Astrophysical Journal",
                 year = "2019",
               volume = "884",
               number = "1",
                pages = "88--95",
             keywords = "Sun: magnetic fields – Sun: photosphere.",
             abstract = "The plasma \β is important in the investigation of 
                         interchanging roles of plasma and magnetic pressure in the solar 
                         atmosphere. It can help to describe features over the photosphere 
                         and their changes at different heights. The goal of this paper is 
                         to obtain the plasma \β variations through the solar corona 
                         during solar cycles 23 and 24. The plasma \β is 
                         reconstructed in different layers of the solar atmosphere. For 
                         this purpose, we use an updated version of the COronal DEnsity and 
                         Temperature model. In this version we selected different features 
                         in the solar atmosphere such as quiet-Sun (QS), faculae, and 
                         active regions. We calculate the \β variations at different 
                         layers in the solar corona (R = 1.14, 1.19, 1.23, 1.28, 1.34, 
                         1.40, 1.46, 1.53, 1.61, 1.74, 1.79, 1.84, and 1.90 Re). In the 
                         photosphere we use temperature values from the FALC model to 
                         obtain plasma \β in QS and faculae. Additionally, variations 
                         of the magnetic and kinetic pressure were modeled during the last 
                         solar cycles at coronal heights.",
                  doi = "10.3847/1538-4357/ab40af",
                  url = "http://dx.doi.org/10.3847/1538-4357/ab40af",
                 issn = "0004-637X",
                label = "lattes: 2768849231719678 4 
                         Rodr{\'{\i}}guezG{\'o}mezPalaVieiLago:2019:Pl\&lEv",
             language = "pt",
           targetfile = "rodriguez_plasma.pdf",
        urlaccessdate = "2019, Dec. 10"
}


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