Intensities in stellar spectra of a triplet of SI III.

Abstract

view Abstract Citations (1) References Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Intensities in stellar spectra of a triplet of SI III. Struve, O. ; Elvey, C. T. Abstract It is shown that under certain assumptions the ratios of total absorptions of the members of the Si m triplet (2's-33p), XX 4553, 4568, and 4575, rn stellar spectra, depend upon the form of the absorptioii coefficient. If the latter is caused by radiation damping, then the total absorptions are proportional to the square roots of the labora- tory intensities. If thermal agitation or any other cause produces a flat but extended absorption coefficient, then the total absorptions are directly proportional to the laboratory intensities. Observations of seven stars confirm the square-root relationship. This is in agreement with the assumption that the absorption coefficient is due to radiation damping, and tends to confirm the hypothesis that dish-shaped lines in early type stars are due to rotation and not to an unusual form of the absorption coefficient. The inte~isities in emission were observed in the spark between terminals of fused sificon. The observed ratios are 4.0:2.4: I, while the theoretical rules give 5:3:1. The deviation may be real. It is noted that stellar spectra are relatively more suitable for the study of faint members of multiplets than are laboratory sources. The stellar intensity ratios are independent of the absolute magnitude of the stars Publication: The Astrophysical Journal Pub Date: November 1930 DOI: 10.1086/143280 Bibcode: 1930ApJ....72..267S full text sources ADS |