. . . . . "In astronomy, the G-dwarf problem refers to the apparent discrepancy in the distribution of metallicity levels in stars of different populations as compared to closed box models of galactic chemical evolution. According to closed box models, which represent galaxies without outside non-metallic material inflow, the distribution of metallicity levels in stars should follow a logarithmic curve. This amounts to high and low mass stars having the least metallicity, with G-type stars inbetween. However, these models are inconsistent with Milky Way observations. Other galaxies have been shown to have the same problem. The name comes from G-type stars, which are bright enough to be studied easily, yet are most often found unevolved. This provides an extensive look at relatively young stars. Despite this, the G Dwarf problem has also been observed in K and M dwarfs."@en . . . "G-dwarf problem"@en . . "Problema da an\u00E3 G"@pt . . "In astronomy, the G-dwarf problem refers to the apparent discrepancy in the distribution of metallicity levels in stars of different populations as compared to closed box models of galactic chemical evolution. According to closed box models, which represent galaxies without outside non-metallic material inflow, the distribution of metallicity levels in stars should follow a logarithmic curve. This amounts to high and low mass stars having the least metallicity, with G-type stars inbetween. However, these models are inconsistent with Milky Way observations. Other galaxies have been shown to have the same problem. The name comes from G-type stars, which are bright enough to be studied easily, yet are most often found unevolved. This provides an extensive look at relatively young stars. Despi"@en . "66839694"^^ . . . . "Em astronomia, o problema da an\u00E3 G refere-se \u00E0 aparente discrep\u00E2ncia na distribui\u00E7\u00E3o dos n\u00EDveis de metalicidade em estrelas de diferentes popula\u00E7\u00F5es em compara\u00E7\u00E3o com modelos de caixa fechada de evolu\u00E7\u00E3o qu\u00EDmica gal\u00E1ctica. De acordo com os modelos de caixa fechada, que representam gal\u00E1xias sem entrada de material n\u00E3o met\u00E1lico externo, a distribui\u00E7\u00E3o dos n\u00EDveis de metalicidade nas estrelas deve seguir uma curva logar\u00EDtmica. Isso equivale a estrelas de massa alta e baixa tendo a menor metalicidade, com estrelas de classe G no meio. No entanto, esses modelos s\u00E3o inconsistentes com as observa\u00E7\u00F5es da Via L\u00E1ctea. Outras gal\u00E1xias mostraram ter o mesmo problema. O nome vem de estrelas de classe G, que s\u00E3o brilhantes o suficiente para serem estudadas facilmente, mas na maioria das vezes s\u00E3o encontr"@pt . "2111"^^ . . "1096489188"^^ . "Em astronomia, o problema da an\u00E3 G refere-se \u00E0 aparente discrep\u00E2ncia na distribui\u00E7\u00E3o dos n\u00EDveis de metalicidade em estrelas de diferentes popula\u00E7\u00F5es em compara\u00E7\u00E3o com modelos de caixa fechada de evolu\u00E7\u00E3o qu\u00EDmica gal\u00E1ctica. De acordo com os modelos de caixa fechada, que representam gal\u00E1xias sem entrada de material n\u00E3o met\u00E1lico externo, a distribui\u00E7\u00E3o dos n\u00EDveis de metalicidade nas estrelas deve seguir uma curva logar\u00EDtmica. Isso equivale a estrelas de massa alta e baixa tendo a menor metalicidade, com estrelas de classe G no meio. No entanto, esses modelos s\u00E3o inconsistentes com as observa\u00E7\u00F5es da Via L\u00E1ctea. Outras gal\u00E1xias mostraram ter o mesmo problema. O nome vem de estrelas de classe G, que s\u00E3o brilhantes o suficiente para serem estudadas facilmente, mas na maioria das vezes s\u00E3o encontradas n\u00E3o-evolu\u00EDdas. Isso fornece uma vis\u00E3o abrangente de estrelas relativamente jovens. Apesar disso, o problema da an\u00E3 G tamb\u00E9m foi observado em an\u00E3s K e M."@pt . .