Hostname: page-component-cd9895bd7-lnqnp Total loading time: 0 Render date: 2024-12-12T08:33:07.122Z Has data issue: false hasContentIssue false
  • English
  • Français

Precise Reduction to the Apparent Places of Stars

Published online by Cambridge University Press:  14 August 2015

S. Yumi ,
K. Hurukawa  and
Th. Hirayama
S. Yumi
Affiliation:
International Latitude Observatory, Mizusawa, and Tokyo Astronomical Observatory, Japan
K. Hurukawa
Affiliation:
International Latitude Observatory, Mizusawa, and Tokyo Astronomical Observatory, Japan
Th. Hirayama
Affiliation:
International Latitude Observatory, Mizusawa, and Tokyo Astronomical Observatory, 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.

For a precise reduction to the apparent places of the stars in a uniform system during the 19th and 20th centuries, the ‘Solar Coordinates 1800–2000’ by Herget (Astron. Papers14, 1953) may conveniently be used, because no coordinates of the Sun, referred to the mean equinox of 1950.0, are given in the Astronomical Ephemeris before 1930.

A maximum difference of 0″.0003 was found between the aberrations calculated from both the Astronomical Ephemeris and Herget's Tables for the period 1960–1969, taking into consideration the effect of the outer planets, which amounted to 0″.0109.

The effect of the inner planets on the aberration is estimated to be of the order of 0″.0001 at the most and the correction for the lunar term due to the change in astronomical constants is 0″.00002. It is recommended that the solar coordinates be calculated directly from Newcomb's formulae taking the effects of all the planets into consideration, but the effect concerned with the Moon can be neglected.

Type
Session G: Astrometric Techniques
Information
Symposium - International Astronomical Union , Volume 61: New Problems in Astrometry , 1974 , pp. 319
Copyright
Copyright © Reidel 1974