Open AccessThe evolution of the spectrum of a star during its growth from a nebula
Author(s) -
William E. Wilson
Publication year - 1905
Publication title -
proceedings of the royal society of london. series a, containing papers of a mathematical and physical character
Language(s) - English
Resource type - Journals
eISSN - 2053-9150
pISSN - 0950-1207
DOI - 10.1098/rspa.1905.0040
Subject(s) - nebula , physics , astrophysics , line (geometry) , spectrum (functional analysis) , emission nebula , helium , star (game theory) , astronomy , spectral line , stars , atomic physics , geometry , quantum mechanics , mathematics
In considering the probable evolution of the spectrum of a star in its different stages from a nebula, let us first consider a mass of gas at a sufficiently high temperature to be able to radiate waves of light into the surrounding space. If this mass of gas were sufficiently rare to be transparent to all wave-lengths of light except those which it is itself able to radiate, its spectrum would be a bright-line one. Sir William Huggins was the first to show, in 1864, that many nebulæ gave a simple spectrum of a few bright lines. These lines show the presence of hydrogen and helium. Some other faint lines are also seen, but their origin is at present not known.