Celestial Mechanics and Dynamical Astronomy

, Volume 105, Issue 4, pp 329–336

A Mercury orientation model including non-zero obliquity and librations

Authors

    • Department of Earth & Space Sciences and Institute of Geophysics and Planetary PhysicsUniversity of California

DOI: 10.1007/s10569-009-9234-1

Abstract

Planetary orientation models describe the orientation of the spin axis and prime meridian of planets in inertial space as a function of time. The models are required for the planning and execution of Earth-based or space-based observational work, e.g. to compute viewing geometries and to tie observations to planetary coordinate systems. The current orientation model for Mercury is inadequate because it uses an obsolete spin orientation, neglects oscillations in the spin rate called longitude librations, and relies on a prime meridian that no longer reflects its intended dynamical significance. These effects result in positional errors on the surface of ~1.5 km in latitude and up to several km in longitude, about two orders of magnitude larger than the finest image resolution currently attainable. Here we present an updated orientation model which incorporates modern values of the spin orientation, includes a formulation for longitude librations, and restores the dynamical significance to the prime meridian. We also use modern values of the orbit normal, spin axis orientation, and precession rates to quantify an important relationship between the obliquity and moment of inertia differences.

Keywords

Planets rotation Mercury Gravity

Acknowledgments

This work was supported by NASA Planetary Astronomy grant NNX08AO24G/NNX09AQ69G. Application of the model to MESSENGER mission support is supported by MESSENGER grant NNX07AV78G/NNX09AR45G.

Open Access

This article is distributed under the terms of the Creative Commons Attribution Noncommercial License which permits any noncommercial use, distribution, and reproduction in any medium, provided the original author(s) and source are credited.

Copyright information

© The Author(s) 2009