Abstract
THE mean distribution of the stars with respect to magnitude and galactic latitude derived by Prof. van Rhijn, Miss Joyner, Miss Richmond and myself,1 is expressed through values of log N m. (N m,=number of stars per sq. deg. brighter than m) which for the same latitude, north and south, are the same in all galactic longitudes. The supposition that densities having this characteristic may represent the observed features of stellar distribution assumes the sun to be at the centre of a stellar system having rotational symmetry. Although sufficiently exact for many purposes, this assumption is only a first approximation to the state of affairs in the heavens.
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SEARES, F. Some Systematic Features in the Distribution of Stars. Nature 119, 461–463 (1927). https://doi.org/10.1038/119461a0
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DOI: https://doi.org/10.1038/119461a0