Portal de Periódicos da CAPES

Volcanic geology of Tyrrhena Patera, Mars

1990; American Geophysical Union; Volume: 95; Issue: B5 Linguagem: Inglês

10.1029/jb095ib05p07133

2156-2202

R. Greeley, D. A. Crown,

Geology and Paleoclimatology Research

Tyrrhena Patera is a large, low‐relief volcano located in the southern cratered highlands of Mars on a proposed ring fracture of the Hellas basin. The volcano is composed of four or possibly five principal units, the oldest and most areally extensive of which are suggested to be ash on the basis of their morphology and erosional characteristics. Lava flows are observed in a flank flow unit extending from the central caldera to the southwest and apparently cap the summit region. Models derived from the study of terrestrial pyroclastic flows have been applied to the deposits at Tyrrhena Patera and indicate that the distribution and lengths of the observed deposits are consistent with an origin by the emplacement of gravity‐driven ash flows generated by hydromagmatic or magmatic explosive eruptions. The hydromagmatic case requires considerable quantities of water (∼7.5×10 16 kg); however, at volumetric water flow rates determined by other investigators (∼10 5 m 3 /s) and calculated from the regional slopes in the Hesperia Planum region (∼106 m 3 /s), the amounts necessary could be supplied relatively rapidly in geologic time. Tyrrhena Patera represents the earliest central vent volcanism identified on Mars and may reflect a transition from the flood‐style eruptions which dominated early Martian history. A hydromagmatic origin for Tyrrhena Patera is in agreement with suggested climatic changes on Mars and may explain the absence of this style of volcanism in later eras. Alternatively, a magmatic origin for Tyrrhena Patera implies an evolution in the types of magmas produced on Mars from Hesperian to Amazonian time, during which the prominent shields in the Tharsis region formed.