Abstract
THE continuous spectrum of Nova 452.1934 Herculis has been showing a change in the spectral energy distribution which is hard to explain from the point of view of pure temperature radiation. Fig. 1, curve a, presents the continuous spectrum observed on December 31, 1934, by Barbier, Chalonge and Vasy1, and curve b the spectrum on March 6, 1935. Intermediate curves between these extremes will be found in the same publication. (The dotted line has been added by me.) Nova Geminorum 2 showed, during 1912–13, a similar energy distribution curve with one or even two secondary maxima in the early stage, which gradually disappeared2.
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References
D. Barbier, D. Chalonge, É Vasy, C. R., 201, 128 (1935).
W. H. Wright, Lick Obs. Publ., 14, II. A. Brill, Publ. Astrophys. Obs. Potsdam, 23, 70 (1914).
W. M. Cohn, Z. Phys., 75, 544 (1932). Astron. Nachr., 245, 378 (1932). W. Finkelnburg, Astrophys. J., 80, 313 (1934).
C. J. Anger, Harvard Coll. Obs. Bull., 882 (1931).
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COHN, W. Continuous Spectra of Certain Types of Stars and Nebulæ. Nature 137, 150–151 (1936). https://doi.org/10.1038/137150b0
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DOI: https://doi.org/10.1038/137150b0
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