DPS Pasadena Meeting 2000, 23-27 October 2000
Session 24. Moon and Mercury Posters
Displayed, 1:00pm, Monday - 1:00pm, Friday, Highlighted Tuesday and Thursday, 3:30-6:30pm, C101-C105, C211

[Previous] | [Session 24] | [Next]

[24.02] A Time Dependent Model of Radiative and Conductive Thermal Energy Transport in Planetary Regoliths with Applications to the Moon and Mercury

A.S. Hale (Jet Propulsion Laboratory), B.W. Hapke (University of Pittsburgh)

When considering the problem of thermal energy transfer in the regoliths of airless bodies, both radiative and conductive transfer must be considered. In the past radiative transfer has generally been addressed by adding a T3 term to the conductivity, but this approximation is only valid when the modeled medium is in radiative equilibrium, which is not the case for the near-surface layers of a regolith. To rigorously account for radiative transfer as well as conductive transfer of thermal energy in a regolith, the radiative transfer and heat transfer equations must be solved simultaneously. Hapke (1996) presented a rigorous radiative model, but considered only time-independent cases. As the solar input to any planetary surface is not constant with time, time dependence should be included. We present the first time-dependent thermal energy transfer model which rigorously accounts for radiative transfer. Such a model allows for determination of the thermal inertia of a regolith, as did previous models, but also allows for constraint of a new parameter, which we term the radiative resistivity. Knowledge of this parameter in turn makes estimates of grain size possible from remote observation of surface temperature versus time curves. This model also predicts an enhancement of the conductivity of the regolith of an airless planet during the day when the temperature is high, and a corresponding reduction in its conductivity at night due to the highly temperature dependent nature of radiative energy transfer. In practice, this means that heat is more easily shunted from the surface to depth than would otherwise be the case during the day, but is trapped in the subsurface at night. Our model also predicts that the subsurface polar regions of both the Moon and Mercury may be sufficiently cold to have harbored water ice over geologic time scales.

The author(s) of this abstract have provided an email address for comments about the abstract: Amy.S.Hale@jpl.nasa.gov

[Previous] | [Session 24] | [Next]