@Article{Evangelista:2019:AbDiTr,
               author = "Evangelista, Edgard de Freitas Diniz",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)}",
                title = "Dedu{\c{c}}{\~a}o do limite de Chandrasekhar: uma abordagem 
                         did{\'a}tica dos trabalhos originais do autor",
              journal = "Revista Brasileira de Ensino de F{\'{\i}}sica",
                 year = "2019",
               volume = "41",
               number = "2",
                pages = "e20180167--1--e20180167--6",
             keywords = "Astrophysics, Chandrasekhar Limit, White Dwarfs.",
             abstract = "Os atuais modelos de evolu{\c{c}}{\~a}o estelar estabelecem que 
                         estrelas possuindo at{\'e} cerca de oito vezes a massa do Sol 
                         d{\~a}o origem a an{\~a}s brancas no final de suas vidas. Na 
                         d{\'e}cada de 1920 surgiram trabalhos que descreviam tais objetos 
                         como formados essencialmente por um g{\'a}s de el{\'e}trons e 
                         n{\'u}cleons, de forma que a for{\c{c}}a de sua press{\~a}o de 
                         degeneresc{\^e}ncia equilibrava a contra{\c{c}}{\~a}o 
                         gravitacional, originando corpos est{\'a}veis e de alta 
                         densidade. Na d{\'e}cada de 1930 Subrahmanyan Chandrasekhar 
                         lan{\c{c}}ou sua abordagem ao problema das an{\~a}s brancas em 
                         artigos onde ele deduziu as densidades e a massa m{\'a}xima 
                         permitida para essas estrelas. Tal valor m{\'a}ximo para a massa 
                         {\'e} hoje conhecido como limite de Chandrasekhar e o objetivo 
                         aqui {\'e} analisar os trabalhos originais de seu descobridor, 
                         mostrando de forma did{\'a}tica os passos que levaram {\`a} 
                         dedu{\c{c}}{\~a}o desse importante resultado. ABSTRACT: The 
                         current stellar evolution models establish that stars which have 
                         up to approximately eight times the solar mass yield white dwarfs 
                         at the end of their lifes. Works appeared at the 1920s described 
                         such objects as formed essentially by a gas of electrons and 
                         nucleons, where the force of its degeneracy pressure equalized the 
                         gravitational contraction, giving rise to stable bodies with high 
                         densities. At the 1930s Subrahmanyan Chandrasekhar launched his 
                         approach to the white dwarf problem in papers where he deduced the 
                         densities and the maximum mass allowed for those stars. Such a 
                         maximum value is known nowadays as the Chandrasekhar limit and the 
                         aim here is to analyze the original papers by its discoverer, 
                         presenting in a didactic form the steps which led to the deduction 
                         of that important result.",
                  doi = "10.1590/1806-9126-rbef-2018-0167",
                  url = "http://dx.doi.org/10.1590/1806-9126-rbef-2018-0167",
                 issn = "1806-1117",
                label = "lattes: 9022248252382153 1 Evangelista:2019:AbDiTr",
             language = "pt",
           targetfile = "Evangelista_deducao.pdf",
        urlaccessdate = "27 abr. 2024"
}