Image Details

Choose export citation format:

Determining Titan's Spin State from Cassini RADAR Images

  • Authors: Bryan W. Stiles, Randolph L. Kirk, Ralph D. Lorenz, Scott Hensley, Ella Lee, Steven J. Ostro, Michael D. Allison, Philip S. Callahan, Yonggyu Gim, Luciano Iess, Paolo Perci del Marmo, Gary Hamilton, William T. K. Johnson, Richard D. West, and the Cassini RADAR Team

STILES et al. 2008 The Astronomical Journal 135 1669.

  • Provider: AAS Journals

Caption: Figure 4.

Landmark misregistration error versus latitude and longitude plots for overall best fit (top) and best fit constrained to have constant, synchronous spin rate and no pole wobble (bottom). Vector lengths are in units of 100 m, so that a vector that extends across twenty degrees on the plot actually represents a 2 km error. The tail of the arrow corresponds to the location of the first observation of each landmark. The direction of the arrow is the direction of apparent change in the landmark location. Clearly, including spin rate and pole change parameters improves the fit in a systematic manner.

Other Images in This Article
Copyright and Terms & Conditions