Computer Science
Scientific paper
Oct 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997icar..129..401s&link_type=abstract
Icarus, Volume 129, Issue 2, pp. 401-414.
Computer Science
10
Scientific paper
A variety of techniques have demonstrated that some of the solid bodies of the Solar System have distinct irregular shapes, while the rest have sphere-like equilibrium shapes; a sharp transition exists between the two. Such an abrupt, mass-dependent transition may be explained by the yield strength of material at low temperatures. Gravitational forces in nonequilibrium figures produce structural stresses, and if a body is sufficiently massive to produce differential stresses above the yield strength, then the shape of the body will relax into an equilibrium, sphere-like figure. A solution is obtained herein that allows estimation of the critical size and mass of a body of any composition or, conversely, estimation of the strength properties of real icy and rocky bodies. By use of available data on strength properties of chondrites, the critical radius of an ordinary chondritic body is estimated to be 756 km. The critical radius of a body with the composition of select terrestrial basic rocks is estimated to be 582 km. Each of these figures is between the diameters of Vesta (small body) and the Moon (planetary body). At the temperature of the saturnian system (70 K), the yield strength of icy Hyperion and Mimas (both of which are in the transitional size range) is between 0.38 and 1.4 MPa. The yield strength of Proteus in the neptunian system (30-40 K) is estimated to be 1.62 MPa, illustrating the well-known dependence of yield strength on temperature and corresponding well to available experimental data on the strength properties of water ice. The asteroids 2 Pallas and 1 Ceres, occupying the transitional size range between small and planetary bodies, have estimated yield strengths of 16.0 to 60.2 MPa. These values are much lower than those for ordinary chondrites (about 250 MPa) and are perhaps more appropriate for carbonaceous chondrites.
Slyuta Evgeniy N.
Voropaev Sergey A.
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