Hostname: page-component-745bb68f8f-cphqk Total loading time: 0 Render date: 2025-01-09T07:24:56.605Z Has data issue: false hasContentIssue false
  • English
  • Français

Emission Line Analyses of HBV 475, V1016 CYG, and HM SGE

Published online by Cambridge University Press:  12 April 2016

S. Tamura
S. Tamura*
Affiliation:
Astronomical Institute, Tohoku UniversityAobayama, Sendai 980, Japan

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Results of the high dispersion spectroscopic observations on HBV 475, V1016 Cyg, and HM Sge are presented. Due to yearly observations of HBV 475 since 1981, radial velocities which have been measured from Hα and Hγ can be explained by a bipolar like non-spherical flow combined with the rotation. Highly resolved profiles of Hα, [FeVII]λ6087, [0III] λλ4959,5007, and HeIIλ4686 are obtained from V1016 Cyg and HM Sge as well as HBV 475. Characteristic differences of them can be seen among these symbiotic stars.

Type
Session 3. Physics of Individual Objects
Information
International Astronomical Union Colloquium , Volume 103: The Symbiotic Phenomenon , 1988 , pp. 285 - 286
Copyright
Copyright © Kluwer 1988

References

Iijima, T., Mammario, A., and Margoni, R. 1981, Ap. and Space Sci., 75, 237 Google Scholar