Hostname: page-component-77c89778f8-m8s7h Total loading time: 0 Render date: 2024-07-19T18:20:51.610Z Has data issue: false hasContentIssue false
  • English
  • Français

Computing parallactic refraction for stellar triangulation

Published online by Cambridge University Press:  14 August 2015

Juhani Kakkuri  and
Ossi Ojanen
Juhani Kakkuri
Affiliation:
Finnish Geodetic Institute, Helsinki
Ossi Ojanen
Affiliation:
Finnish Geodetic Institute, Helsinki

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 parallactic refraction correction should be applied to the photographic observations of the light signals carried either by artificial satellites or by meteorological balloons. The correction to the right ascension and declination are made with the equations

where ϕ is the latitude of the observation station, z the zenith distance, α the right ascension, δ the declination and h the hour angle of the light signal. Parallactic refraction is denoted by Δζ.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 89: Refractional Influences in Astrometry Andgeodesy , 1979 , pp. 275 - 279
Copyright
Copyright © Reidel 1979 

References

3. References

Kakkuri, Juhani (1973), Stellar Triangulation with Balloon-Borne Beacons. Ann. Acad. Sci. Fenn. A. III, 113. Helsinki.Google Scholar
Oterma, Liisi (1960), Computing the Refraction for the Väisälä Astronomical Method of Triangulation. Ast. Opt. Inst. Turku Univ. 20. Turku.Google Scholar