are
large enough so that models with no discontinuity are possible. For Uranus
a discontinuity is required, however. The limits on the size and position of
this discontinuity are presented and the implications for the compostion are
discussed.
More Random Models of Uranus and Neptune
M. Podolak (Tel Aviv University), J. I. Podolak (Struma 5), M. S. Marley (New Mexico State Univ.)
Uncertainties in the composition and thermal structure of Uranus and Neptune
make it desirable to try to calculate the limits for the density distribution
inside these planets which are, as much as possible, independent of other
assumptions. To this end Marley et al. (1995) computed Monte Carlo models
where the density distribution was allowed to be random, subject to the constraint
that the density increase monotonically towards the center. They found that
a density jump was required for both planets at a radius of about 0.6 to 0.7 of the
total radius. We have used a more efficient algorithm to explore the parameter
space, and to find what limits can be set on the density discontinuity. For
Neptune we find that the uncertainties in the measured value of are
large enough so that models with no discontinuity are possible. For Uranus
a discontinuity is required, however. The limits on the size and position of
this discontinuity are presented and the implications for the compostion are
discussed.
Marley, M. S., Gomez, P., and Podolak, M. (1995). Monte Carlo models for Uranus
and Neptune. J. Geophys. Res. 100:23,349-23,353.