# M m log l l t ef r 10 10 t c ρ clog pc qc qe ρρ c

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M M log L L T ef R/ 10 10 T c ρ c log P c q c q e ρ ρ c ρ (K) (cm) (10 6 K) (g / cm 3 ) (dina / cm 2 ) (g / cm 3 ) 60 5,70 48200 70,96 39,28 1,93 16,12 0,74 0 0,08 24 15 4,29 31500 32,89 32,75 5,48 16,44 0,40 0 0,20 27 5 2,77 18200 17,18 26,43 19,0 16,84 0,23 0 0,47 8 2 1,26 9800 10,30 21,09 47,0 17,21 0,13 0 0,87 54 1,75 1,03 8900 9,683 20,22 66,5 17,25 0,11 0 0,92 72 1,5 0,76 7800 9,141 19,05 76,7 17,28 0,07 0 0,94 82 1,2 0,34 6300 8,650 16,67 85,7 17,26 0,01 10 - 7 0,89 97 1 -0,04 5600 6,934 14,42 82,2 17,17 0 0,0035 1,43 57 0,3 -1,96 3500 2,054 7,59 107 17,05 0 1 16,5 0,15 0,08 -3,80 2100 0,650 3,30 775 17,83 0 1 139 0,18 431
dentro da precis˜ao pr´ e-determinada. Este m´ etodo, de transformar um pro- blema n˜ao linear em um linear, chama-se de m´ etodo de Newton—Raphson [Isaac Newton (1642-1727) e Joseph Raphson (1648-1715)]. No m´ etodo de Henyey, a cada intera¸c˜ ao corre¸c˜ oes para todas as vari´ aveis em todos os pon- tos s˜ao calculados simultaneamente [Louis George Henyey (1910-1970), J.E. Forbes e Nancy L. Gould 1964, Astrophysical Journal, 139, 306]. Nosso c´alculo para estrelas esf´ ericas consiste ent˜

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