论文信息 - The tectonics of Ganymede

The tectonics of Ganymede

The surface of Ganymede, the largest icy jovian satellite, is composed of two distinct terrain types showing abundant evidence of global-scale tectonics. There is geological evidence consistent with the formation of younger bright terrain by the emplacement of relatively clean ice into rift zones developed in the more silicate-rich dark terrain.

[1] S. Solomon. On volcanism and thermal tectonics on one-plate planets , 1978 .

[2] B. Lucchitta. Grooved terrain on Ganymede , 1980 .

[3] H. Melosh,et al. Evolution of planetary lithospheres: Evidence from multiringed structures on Ganymede and Callisto , 1980 .

[4] J. Head,et al. Internal processes affecting surfaces of low‐density satellites: Ganymede and Callisto , 1979 .

[5] S. Squyres. Volume changes in Ganymede and Callisto and the origin of grooved terrain , 1980 .

[6] Bradford A. Smith,et al. The Jupiter System Through the Eyes of Voyager 1 , 1979, Science.

[7] S. Squyres. Surface temperatures and retention of H2O frost on Ganymede and Callisto , 1980 .

[8] Steven W. Squyres,et al. The topography of Ganymede's grooved terrain , 1981 .

[9] J. Head,et al. Viscous relaxation of impact craters on icy planetary surfaces - Determination of viscosity variation with depth , 1981 .

[10] T V Johnson,et al. The Galilean Satellites and Jupiter: Voyager 2 Imaging Science Results , 1979, Science.