Stellar Structure


BY an unaccountable slip, a numerical error crept into our recent communication1 concerning the nuclei of planetary nebulæ. With the assumed data for a typical nucleus, it is the superficial area which is 1/43 of the sun's. With mass equal to the sun, the mean density comes out 400 gm./cm.3, and with the probable mass 80 suns, as 32,000 gm./cm.3. This is still high enough to justify the classification of these stars with the white dwarfs; but degeneracy of the gas appears to be only beginning, rather than far advanced.

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  1. 1

    NATURE, May 2, p. 661.

  2. 2

    Publications Astron. Soc. Pac., 38, 302; 1926.

  3. 3

    The Observatory April.

  4. 4

    Zeits. f. Astrophysik, 2, p. 153; 1931.

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RUSSELL, H., ATKINSON, R. Stellar Structure. Nature 127, 894 (1931).

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