| Автор | Durham, WB |
| Автор | Stern, LA |
| Дата выпуска | 2001 |
| dc.description | ▪ Abstract The icy moons of the outer solar system have not been quiescent bodies, in part because many have a substantial water component and have experienced significant internal heating. We can begin to understand the thermal evolution of the moons and the rate of viscous relaxation of surface topography because we now have good constraints on how ice (in several of its polymorphic forms) flows under deviatoric stress at planetary conditions. Details of laboratory-derived flow laws for pure, polycrystalline ice are reviewed in detail. One of the more important questions at hand is the role of ice grain size. Grain size may be a dynamic quantity within the icy moons, and it may (or may not) significantly affect rheology. One recent beneficiary of revelations about grain-size-sensitive flow is the calculation of the rheological structure of Europa's outer ice shell, which may be no thicker than 20 km. |
| Формат | application.pdf |
| Издатель | Annual Reviews |
| Копирайт | Annual Reviews |
| Название | RHEOLOGICAL PROPERTIES OF WATER ICE—APPLICATIONS TO SATELLITES OF THE OUTER PLANETS <sup>1</sup> |
| DOI | 10.1146/annurev.earth.29.1.295 |
| Print ISSN | 0084-6597 |
| Журнал | Annual Review of Earth and Planetary Sciences |
| Том | 29 |
| Первая страница | 295 |
| Последняя страница | 330 |
| Аффилиация | Durham, WB; Lawrence Livermore National Laboratory, University of California, Livermore, California 94550; e-mail: durham@llnl.gov |
