Abstract
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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References
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RUSSELL, H., ATKINSON, R. Stellar Structure. Nature 127, 894 (1931). https://doi.org/10.1038/127894b0
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DOI: https://doi.org/10.1038/127894b0
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