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@Article{RodríguezGómezPalaVieiDalL:2019:PlBeEv,
               author = "Rodr{\'{\i}}guez G{\'o}mez, Jenny Marcela and Palacios, Judith 
                         and Vieira, Luis Eduardo Antunes and Dal Lago, Alisson",
          affiliation = "{Skolkovo Institute of Science and Technology (Skoltech)} 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 beta evolution through the solar corona during solar 
                         cycles 23 and 24",
              journal = "Astrophysical Journal",
                 year = "2019",
               volume = "884",
               number = "1",
                pages = "e88",
                month = "Oct.",
             keywords = "Sun: magnetic fields, Sun: photosphere.",
             abstract = "The plasma beta 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 beta variations through the solar corona during solar 
                         cycles 23 and 24. The plasma beta 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 beta 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 R-circle dot). In the photosphere we 
                         use temperature values from the FALC model to obtain plasma beta 
                         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 and 1538-4357",
             language = "en",
           targetfile = "gomez_plasma.pdf",
        urlaccessdate = "17 abr. 2021"
}


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