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Some observational appearances of m=1 density waves in Be star disks

Published online by Cambridge University Press:  26 May 2016

Atsuo T. Okazaki
Atsuo T. Okazaki*
Affiliation:
College of General Education, Hokkai-Gakuen University, Toyohira-ku, Sapporo 062, Japan

Extract

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One-armed (i.e., m = 1) density waves are the only global waves in nearly Keplerian disks (Kato 1983). Their frequencies are much smaller than the angular frequency of disk rotation. Based on this theory, Okazaki (1991) proposed that the long-term V/R variations of Be stars are phenomena caused by the global m = 1 oscillations in the equatorial disks. Hummel and Hanuschik (1993) showed that line profiles of disks with m = 1 perturbation patterns are in agreement with the observed V/R variability.

Type
6. Be Stars: Circumstellar Environment
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 380 - 381
Copyright
Copyright © Kluwer 1994 

References

Hummel, W., and Hanuschik, R.W.: 1993, these proceedings Google Scholar
Kato, S.: 1983, Publ. Astron. Soc. Japan 35, 249 Google Scholar
Kogure, T., Suzuki, M.: 1984, Publ. Astron. Soc. Japan 36, 191 Google Scholar
Okazaki, A.T.: 1991, Publ. Astron. Soc. Japan 43, 75 Google Scholar