The topography and morphology of low shields and associated landforms of plains volcanism in the Tharsis region of Mars

Arecibo radar imagery of Mars: The major volcanic provinces

“…Finally, in an unrelated note, we point to the region of Syria Planum between 255-265°E and 10-20°S, where spacecraft imagery has identified clusters of small shields, vents, and lava flows (Hodges and Moore, 1994;Baptista et al, 2008;Hauber et al, 2009;Richardson et al, 2010). Our imagery (Fig.…”

“…East of the South Volcanic Field is a contiguous area of moderately high radar brightness that extends to the barrier of Noctis Fossae (7-K), at the west edge of the Syria Rise. This bright region includes: a second cluster of small shields just west of the Fossae at 250.5°E, 5°S (Hauber et al, 2009); a shield-free but flow-covered plains region separating this cluster from the South Volcanic Field; and an E/W-trending arc of vents centered at 248°E, 5°S (Hauber et al, 2009). The radar imagery shows that this entire complex of small vents and lava plains south of Pavonis Mons has moderate to high small-scale surface roughness, with the roughest surfaces being in the South Volcanic Field proper.…”

“…Strictly speaking, the Hodges-Moore apron refers to the near-shield lavas that flow north around the eastern base of Pavonis Mons, wrap around the older Pavonis northeast apron, and combine with flows from the south end of the Ascraeus south apron to produce the prominent bright flow lobe (7-B) extending northwest down the Tharsis west slope (Section 4.6). However, the large radar-bright feature (7-D) also encompasses a large cluster of small shields and vents between Pavonis Mons and Noctis Fossae (Hauber et al, 2009) as well as the Ascraeus Mons small-vent field just to its north (Section 4.3). On the east side, the very bright Pavonis east apron feature blends in with the moderately bright lavas flowing down the Tharsis east slope and spreading across the East Tharsis plains (Section 4.7).…”

Volcanism and tectonism across the inner solar system: an overview

“…Their basal diameters range from a few kilometres to a few tens of kilometres, and they frequently have summit elevations of up to several hundred metres and flank slopes of less than 58 Bleacher et al 2009;Hauber et al 2009;Richardson et al 2013). These shield volcanoes are typical of plains-style volcanism (Greeley 1982).…”

“…9d), defined here as scoria/cinder and tephra cones and tuff rings, have only been observed on Mars since the availability of high-resolution imagery in the following areas: Pavonis Mons (Keszthelyi et al 2008), Ascraeus Mons (Mouginis-Mark & Christensen 2005), Syria Planum (Hauber et al 2009), Ulysses Fossae (Brož & Hauber 2012), Utopia Planitia (Lanz et al 2010), Nili Patera (Skok et al 2010) and the NephentesAmenthes region (Skinner & Tanaka 2007;Brož & Hauber 2013). Nevertheless, their possible existence in some locations had been reported earlier (e.g.…”