A self-replication model for long channelized lava flows on the Mars plains

• Published in: Journal of Geophysical Research - Planets Vol. 113; no. E5; pp. E05003 - n/a
• Main Authors: Baloga, S. M., Glaze, L. S.
• Format: Journal Article
• Language: English
• Published: Washington, DC American Geophysical Union 01-05-2008; Blackwell Publishing Ltd
• Subjects: channel; Earth sciences; Earth, ocean, space; Effusive volcanism; Eruption mechanisms and flow emplacement; Exact sciences and technology; lava flow; Lava rheology and morphology; Planetary Sciences; Planetary volcanism; self-replicating; Solid Surface Planets; Volcanism; Volcanology; Narrows; New York; United States; channel; self-replicating; lava flow; emplacement; models; growth rates; exhibits; velocity; North America; crust; duration; Persistence; Earth; drill cores; crustal growth; Mars; dynamics; lava; viscosity; channels; buildings; plains; lava flows; transient phenomena; flow
• ISSN: 0148-0227; 2156-2202
• DOI: 10.1029/2007JE002954

A model is presented for channelized lava flows emplaced by a self‐replicating, levee‐building process over long distances on the plains of Mars. Such flows may exhibit morphologic evidence of stagnation, overspills, and upstream breakouts. However, these processes do not inhibit the formation and persistence of a prominent central channel that can often be traced for more than 100 km. The two central assumptions of the self‐replication model are (1) the flow advances at the average upstream velocity of the molten core and (2) the fraction of the lava that travels faster than the average upstream velocity forms stationary margins in the advancing distal zone to preserve the self‐replication process. For an exemplary 300 km long flow north of Pavonis Mons, the model indicates that ∼8 m of crust must have formed during emplacement, as determined from the channel and levee dimensions. When combined with independent thermal dynamic estimates for the crustal growth rate, relatively narrow constraints are obtained for the flow rate (2250 m3 s−1), emplacement duration (600 d), and the lava viscosity of the molten interior (106 Pa s). Minor, transient overspills and breakouts increase the emplacement time by only a factor of 2. The primary difference between the prodigious channelized Martian flows and their smaller terrestrial counterparts is that high volumetric flow rates must have persisted for many hundreds of days on Mars, in contrast to a few hours or days on Earth.