Vertical distribution of temperature and density in a planetary ring
Jürgen Schmidt 1,
Heikki Salo 2,
Olaf Petzschmann 1 and
Frank Spahn 1
Received 4 January 1999 / Accepted 21 January 1999
We model temperature and density profiles for a dilute planetary ring, based on the hydrodynamic balance equations for momentum and energy of granular flows. Within our approximation the ring consists of inelastic smooth spheres of unique size and mass, while the fluxes of mass, momentum and energy are linear functions of the gradients of density, velocity and temperature. The resulting system of coupled differential equations leads to temperature and density profiles, which we compare to the results of a triaxial kinetic approach to the dynamics of a planetary ring. We find that both approaches agree fairly well in the elastic limit. Further, we carry out event driven N-particle simulations of a ring, subject to the conditions of the theoretical model. The simulated profiles are then compared to the theoretical ones: for the density a good agreement is found for both theoretical approaches, but the simulated temperature profiles increase monotonically with vertical distance whereas the theoretical profiles always have a turnover at some distance from the mid plane. This disagreement is likely to be connected to the vertical dependence of the velocity ellipsoid, which is not taken into account in the theoretical treatments.
Key words: hydrodynamics methods: N-body simulations planets and satellites: general
Send offprint requests to: Juergen Schmidt
Correspondence to: Juergen Schmidt, Universitaet Potsdam, Institut fuer Physik, Lehrstuhl Nichtlineare Dynamik, Am Neuen Palais 10, Haus 19, D-14415 Potsdam, Germany, Tel. +49 331 977 1364, Fax. +49 331 977 1142, e-mail: firstname.lastname@example.org
This article contains no SIMBAD objects.
© European Southern Observatory (ESO) 1999
Online publication: April 19, 1999