Orientation of the moon by numerical integration

Abstract

The differential equations of rotational motion of the Moon are solved by numerical integration methods. Euler's dynamical equations transformed to a convenient form are treated by techniques analogous to ordinary orbit determination procedures. The proposed method is fully consistent with the ephemeris of the Moon and can utilize a variety of observational material for the solution of the selected parameters. The parameters are grouped into three distinct groups, namely: --The physical libration angles of the Moon and their time rates at an arbitrary initial epoch. --Physical constants featuring the principal moments of ineria of the Moon. --Parameters associated with the particular observational material being used.