This article is about the volcanic province on Mars. For other uses, seeElysium (disambiguation).
Elysium
Colorized topographic map of Elysium and its surroundings, from theMOLA instrument ofMars Global Surveyor. The shield volcanoElysium Mons is at center, with the smaller volcanoesHecates Tholus andAlbor Tholus to its upper and lower right, respectively.
The southeastern portion of the province is geochemically distinct from the northwest.[5] The southeast is composed of sedimentary and porous rocks.[6] The majority of the southeastern portion is made up ofAmazonian-Hesperian volcanic units. Most of the remaining southeastern volcanic units are late Amazonian in nature.[5] In recent history, there were significant groundwater deposits in the region.[7]
It has been hard to study the composition of this province, due to the layer of dust that sits on top of the crust. Investigations in relatively dust-free regions indicate that it is made primarily of high-calciumpyroxene andolivine.[8][9] To a lesser degree, the province is made up ofhematite andhydrated silica, among other things.[8] There are no strong magnetic fields in the region.[9] There are some extant near-surfaceglacial deposits in the caldera of Hecates Tholus, a volcano in the province.[10]
The southeastern portion of the province is approximately 0.85 billion years younger than the northwestern.[5] The region as a whole has been volcanically active for at least 3.9 billion years, with a peak 2.2 billion years ago, although activity has decreased considerably in the last billion years.[11]Crater counting done on thelava flows in the southern region show low cratering rates, which would indicate younger volcanic activity, as recent as 10 Myr.[12] The most recent volcanic activity dates to 2 million years ago.[6] The southeastern portion overlaps with Cerberus Fossae; features in this region are thought to have formed due to volcanic and water-related processes, such asphreatomagmatism, relict ice flows, and interactions between lava and water.[5] In general, many flow units in Elysium Planitia (such asRahway Valles andMarte Vallis) are thought to have their origins in lava originating from this region.[13]
Hecates Tholus erupted ~350 million years ago, with glacial deposits in the resulting caldera dating between 5 and 24 million years ago.[10] Craters in the region are not generally typical of impacts; rather, they are thought to have formed due to explosive volcanism or collapse due to subsurface lava withdrawal.[3]
Elysium contains numerous lava flow units with variable histories as well as volcanic andfluvial channels.[14] The three major volcanoes of the region sit on top of a 1700 x 2400 km broad dome.[14] The summit of Hecates Tholus shows evidence ofpyroclastic activity.[14] Martian volcanism has been dominated byeffusive eruption styles and there is limited evidence to support widespread explosive or pyroclastic volcanic eruptions on Mars.[15]
Elysium Mons is approximately 1.5 times as steep as any other Martian volcano at approximately 7-7.5°.[16][17] The caldera at the summit of Elysium Mons is approximately 13.5 km in diameter.[16][18] Extending past the rim of this central caldera are at least 18 sinuous channels thought to be the remnants of collapsedlava tubes and lava channels.[16]
The Elysium volcanic province was first noticed as a distinct Martian region as a result of data obtained from theMariner 9 mission, in the 1970s.[19][20] TheViking orbiter noted that volcanic province of Elysium experienced more diverse types of volcanism than the Tharsis volcanic region.[21] In 2004,ESA'sMars Express orbiter'sHRSC observed the volcanoes in the region.[22][10] The InSight Lander landed just south of the province in 2018,[9] in Elysium Planitia, and has detectedmarsquakes emanating from this region.[23][24] The main science goals of the lander are to monitor the level of seismic activity occurring on Mars and to understand how Mars formed and how the planet has been evolving ever since.[25][26][27]
Troughs to the east of Albor Tholus, as seen byHiRISE under the HiWish program
Portion of a trough (fossa) in Elysium, as seen by HiRISE under the HiWish program (blue indicates probably seasonal frost)
A Cerberus Fossae trough, as seen from THEMIS
Wind-blown material darkens areas around aCerberus Fossae trough (scale bar for HiRISE image is 500 m)
The Cerberus Fossae, as seen by HiRISE (scale bar is 1.0 km)
TheElysium Fossae, as seen by HiRISE (click on image to see layers)
Two views of theHephaestus Fossae, as seen by HiRISE (picture on right lies to the top (north) of other picture). Fossae often form by material moving into an underground void.
^Mouginis-Mark, Peter J.; Wilson, Lionel; Head, James W.; Brown, Steven H.; Lynn Hall, J.; Sullivan, Kathryn D. (1984-04-01). "Elysium planitia, mars: Regional geology, volcanology, and evidence for volcano-ground ice interactions".Earth, Moon, and Planets.30 (2):149–173.Bibcode:1984EM&P...30..149M.doi:10.1007/BF00114309.ISSN1573-0794.S2CID120632318.
^abcMouginis-Mark, Peter J.; Wilson, Lionel; Head, James W.; Brown, Steven H.; Lynn Hall, J.; Sullivan, Kathryn D. (1984-04-01). "Elysium planitia, mars: Regional geology, volcanology, and evidence for volcano-ground ice interactions".Earth, Moon, and Planets.30 (2):149–173.Bibcode:1984EM&P...30..149M.doi:10.1007/BF00114309.ISSN1573-0794.S2CID120632318.
^McCauley, J. F.; Carr, M. H.; Cutts, J. A.; Hartmann, W. K.; Masursky, Harold; Milton, D. J.; Sharp, R. P.; Wilhelms, D. E. (1972-10-01). "Preliminary mariner 9 report on the geology of Mars".Icarus.17 (2):289–327.Bibcode:1972Icar...17..289M.doi:10.1016/0019-1035(72)90003-6.ISSN0019-1035.
^Mouginis-Mark, Peter J.; Wilson, Lionel; Head, James W.; Brown, Steven H.; Lynn Hall, J.; Sullivan, Kathryn D. (1984-04-01). "Elysium planitia, mars: Regional geology, volcanology, and evidence for volcano-ground ice interactions".Earth, Moon, and Planets.30 (2):149–173.Bibcode:1984EM&P...30..149M.doi:10.1007/BF00114309.ISSN1573-0794.S2CID120632318.
