![]() We present an overview of the formation of Jupiter and its associated circumplanetary disk. The results indicate that in the case of planetesimals which are A possible implementation of a porosity parametrization and model is presented and applied to the collision of two porous agglomerates in three dimensions. Before damage occurs they have to be compacted first. Porous materials, however, behave differently in collisions. The planetesimals in the early solar nebula presumably had a highly porous structure. In order to simulate collisions between planetesimals, the model is changed slightly. The validation of the damage model is performed with the comparison to an impact experiment. The results are compared to the theoretical values given by the Grady-Kipp damage model. The implementation of the damage model is tested using the simulation of a two dimensional tensile rod. The required equations are implemented in an existing parallel SPH code and tested either by numerical tests or validated against experimental measurements: The code is used to model the collision of two dimensional perfect elastic and plastic cylinders. By additionally using a statistical damage model, the method can be applied to the simulation of brittle materials such as basaltic rocks. In order to simulate collisions between planetesimals, the SPH method can be extended to the simulation of elasto-plastic materials. One of the major problems of terrestrial planet formation is the growth from metre-sized protoplanetesimals to larger planetesimals which interact mainly gravitationally. To problems in both terrestrial and gas giant planet formation is presented.
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |