Chronology, Eruption Duration, and Atmospheric Contribution of the Martian Volcano Apollinaris Patera

Shallow radar (SHARAD) sounding observations of the Medusae Fossae Formation, Mars

“…Micron-sized particles may be carried farther by the wind (Wilson and Head, 2007). Possible sites of explosive volcanism and ash deposits on Mars include Alba Patera (MouginisMark et al, 1988), Apollinaris Patera (Robinson et al, 1993), the summit of Arsia Mons (Mouginis-Mark, 2002) and Tyrrhena and Hadriaca Paterae (Greeley and Crown, 1990;Crown and Greeley, 1993). One unresolved problem with the volcanic origin hypothesis for the MFF is the lack of identified source regions, although it has been suggested that Tharsis-related volcanism was a major contributor (Hynek et al, 2003;Edgett and Malin, 2000).…”

Volcanism on the Red Planet: Mars

“…What is the chemical diversity of lavas on Mars, and is there a correlation between volcano morphology and chemistry? Most investigators attribute differences among volcanic features to interaction of the magma with near-surface volatiles or other eruption parameters Crown and Greeley, 1993;Robinson et al, 1993;Wilson and Head, 1994). Thermal Emission Spectrometer (Christensen et al, 1992) data from Mars Global Surveyor, other remote sensing data, and measurements made by landers might resolve the issue of chemical diversity of Martian volcanic rocks.…”

Volcanism and tectonism across the inner solar system: an overview

“…The edifice is about 180 km in diameter and rises up to 3.2 km. Based on its relief, surface texture and degraded friable materials, it is likely to be composed of pyroclastic material (Robinson et al 1993;Crumpler et al 2007). Apollinaris Mons appears to have been active during the Noachian and Hesperian periods (Werner 2009;Tanaka et al 2014), which may have included long-lived hydrothermal activity (El Maarry et al 2012).…”