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SPECTROSCOPIC CHANGES IN THE SUSPECTED X-RAY SOURCE X PERSEI
A. P. COWLEY, D. B. McLAUGHLIN, J. TONEY and D. J. MacCONNELL
Publications of the Astronomical Society of the Pacific
Vol. 84, No. 502 (December 1972), pp. 834-838
Published by: Astronomical Society of the Pacific
Stable URL: http://www.jstor.org/stable/40675317
Page Count: 5
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Spectrograms from 1913 to the present show X Per to have bright H lines that are variable in structure, velocity, and intensity. At times the spectrum is veiled and very few features can be distinguished. During some phases emission of Fe ii, Ti ii, He i, and He ii are seen.Very weak, broad absorption lines suggest the underlying star is near O9. No periodicities are suggested by our data, although we cannot rule out periods shorter than a few months.The slowly changing velocity of the He i absorption lines is particularly difficult to interpret.
Publications of the Astronomical Society of the Pacific © 1972 The University of Chicago Press