Evolution of Martian Lava Flow Fields: Investigations of Pahoehoe-like Flow Morphologies in the Tharsis and Elysium Volcanic Provinces

NASA Mars Data Analysis Program

Start Date: 09/01/2022
Project #: 1876
End Date: 08/31/2025
Award #: 80NSSC22K1085

PSI Personnel

Non PSI Personnel: Steven Anderson (UNCo), Stephen Baloga (Proxemy Res), Stephen Scheidt (Howard), Brent Garry (GSFC)

Project Description

Volcanism is a dominant process forming the surfaces of the terrestrial planets. On Earth, basaltic lava flow fields often consist of diverse lava flow types; Hawaiian and other flow fields exhibit complex assemblages of a’a and pahoehoe flow textures. A’a flows have been widely used as analogues for planetary flows given their simpler shapes, larger dimensions, and well-developed central channels with lateral levees, as well as visibility in early spacecraft datasets. Because of this, there are significant knowledge gaps in our understanding of other lava flow processes and their roles in the evolution of Martian volcanic centers. Recent studies of Martian volcanoes have revealed flow features indicative of processes common to terrestrial pahoehoe lava flows. High-resolution imaging and topographic datasets can now be used to characterize diagnostic details of pahoehoe-like flow emplacement processes that occur in a number of locations with recent Martian volcanism.

We will study the morphologic varieties, topographic attributes, and spatial and temporal contexts of pahoehoe-like flows in a series of Martian lava flow fields in order to address the following: What do pahoehoe flow morphologies indicate about flow emplacement styles and rates? What do the morphologic diversity, spatial and temporal distributions, and volcanic settings of paheohoe-like flow features indicate about the evolution of Martian flow fields? and How do evolutionary patterns in flow field development compare at different sites?

The targeted study areas include: 1) southern Tharsis, including flow fields of the southwest rift apron of Arsia Mons, 2) eastern Tharsis, including rift apron flow fields adjacent to Pavonis and Ascraeus Montes, and 3) southern Elysium, particularly along the dichotomy boundary contact.

Task 1. Catalogue of Flow Morphologies: For each study area, we will compile a comprehensive catalog of pāhoehoe-like flow features, characterize their volcanic settings, and identify possible source vents. In a subset of the larger population using CTX and HiRISE images and DTMs, we will outline flow margins, document textural/morphologic variations, measure longitudinal and cross-sectional profiles, and map surface planform distributary patterns.

Task 2. Spatial Distribution and Chronology: We will analyze spatial distributions of the different types of pahoehoe-like morphologies documented with respect to location in the flow field/volcanic province, relative to other volcanic features (including potential vents), and along any identified distributary pathways. We will select representative areas of pahoehoe-like flows in each flow field and derive absolute model age estimates from superposed craters, providing chronologic constraints on pahoehoe flow emplacement within the different regions of interest.

Task 3. Synthesis: Comparison of Martian Flow Fields: Robust interpretations of flow emplacement styles combined with documentation of their spatial and temporal distributions will constrain the volcanic evolution of lava flow fields in the Tharsis and Elysium provinces. This work will examine the context of and patterns in pahoehoe-like flow emplacement and document the overall significance of low effusion rate volcanism. This work will directly address knowledge gaps in our understanding of the development of Martian volcanic centers.

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