Venus

Venus length-of-day variations are due primarily to the exchange of angular momentum between the atmosphere and the solid planet. A time history of spin rate measurements can therefore provide crucial constraints on the atmospheric dynamics of Venus, enabling key tests of hypotheses related to the superrotation or planet-scale atmospheric structures. We have been obtaining measurements for over a decade. Our initial data indicate that Venus clearly exhibits length-of-day variations. Additional observations are needed to measure daily, seasonal, and secular variations in the rotation rate.

We are also characterizing the evolution of the spin axis orientation, which will provide a direct measurement of the moment of inertia of Venus, an unmeasured yet fundamental constraint on models of the interior. While we have detected the precession, additional observations are needed to secure a measurement with smaller uncertainties. Understanding the obliquity of Venus is also important as it may be excited by mantle convection, volcanic or seismic activity, resurfacing, or atmospheric changes.

This project requires small amounts of telescope time (less than 1 hour per measurement) on the Goldstone 70-m antenna (DSS-14) and the Green Bank Telescope (GBT). However, progress has been hampered by difficulties in securing DSS-14 antenna time, frequent hardware failures, and the necessity to obtain observations at a variety of geometries. A table documents the history of attempted measurements and their outcomes.

Results of our observations to date were presented at the 2012 DPS meeting, 2013 AAS meeting, and 2016 DPS meeting.