Hostname: page-component-77c89778f8-fv566 Total loading time: 0 Render date: 2024-07-18T06:52:43.111Z Has data issue: false hasContentIssue false
  • English
  • Français

Notes on Equinox Motion and Corrections to Precession

Published online by Cambridge University Press:  12 April 2016

T. C. Van Flandern
T. C. Van Flandern*
Affiliation:
U.S. Naval Observatory, Washington, D.C., U.S.A.

Extract

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.

The coordinate system defined by the locations of distant galaxies should be an inertial coordinate system. Until that system becomes better observed, we must use the stars of our own Galaxy, and make certain assumptions in order to achieve an inertial system. Basically, we assume that the stellar proper motions consist of a component due to galactic rotation (a function of distance from the galactic center), a component due to solar motion, and a random component, peculiar to each star. The random component should not cause the star system as a whole to rotate in any particular direction – in other words, the sum of the random components of proper motion will be zero (to within their standard deviation) in every direction.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 9: The IAU System of Astronomical Constants , October 1971 , pp. 182 - 185
Copyright
Copyright © Reidel 1971

References

Fricke, W.: 1967a, Astron. J. 72, 642.CrossRefGoogle Scholar
Fricke, W.: 1967b, Astron. J. 72, 1368.CrossRefGoogle Scholar
Martin, C. F. and Van Flandern, T. C.: 1970, Science 168, 246.Google Scholar
Spencer-Jones, H.: 1939, Monthly Notices Roy. Astron. Soc. 99, 541.Google Scholar