Hesperian

This article is about the Mars geologic system and time period. For other senses, see Hesperia.
Hesperian
3700 – 3000 Ma (upper bound uncertain – between about 3200 and 2000 million years ago)
MOLA colorized relief map of Hesperia Planum, the type area for the Hesperian System. Note that Hesperia Planum has fewer large impact craters than the surrounding Noachian terrain, indicating a younger age. Colors indicate elevation, with red highest, yellow intermediate, and green/blue lowest.
Chronology
SubdivisionsEarly Heperian
Late Hesperian
Usage information
Celestial bodyMars
Time scale(s) usedMartian Geologic Timescale
Definition
Chronological unitPeriod
Stratigraphic unitSystem
Type sectionHesperia Planum

The Hesperian is a geologic system and time period on the planet Mars characterized by widespread volcanic activity and catastrophic flooding that carved immense outflow channels across the surface. The Hesperian is an intermediate and transitional period of Martian history. During the Hesperian, Mars changed from the wetter and perhaps warmer world of the Noachian to the dry, cold, and dusty planet seen today.[1] The absolute age of the Hesperian Period is uncertain. The beginning of the period followed the end of the Late Heavy Bombardment[2] and probably corresponds to the start of the lunar Late Imbrian period,[3][4] around 3700 million years ago (Mya). The end of the Hesperian Period is much more uncertain and could range anywhere from 3200 to 2000 Mya,[5] with 3000 Mya being frequently cited. The Hesperian Period is roughly coincident with the Earth's early Archean Eon.[2]

With the decline of heavy impacts at the end of the Noachian, volcanism became the primary geologic process on Mars, producing vast plains of flood basalts and broad volcanic constructs (highland paterae).[6] By Hesperian times, all of the large shield volcanoes on Mars, including Olympus Mons, had begun to form.[7] Volcanic outgassing released large amounts of sulfur dioxide (SO2) and hydrogen sulfide (H2S) into the atmosphere, causing a transition in the style of weathering from dominantly phyllosilicate (clay) to sulfate mineralogy.[8] Liquid water became more localized in extent and turned more acidic as it interacted with SO2 and H2S to form sulfuric acid.[9][10]

By the beginning of the Late Hesperian the atmosphere had probably thinned to its present density.[10] As the planet cooled, groundwater stored in the upper crust (megaregolith) began to freeze, forming a thick cryosphere overlying a deeper zone of liquid water.[11] Subsequent volcanic or tectonic activity occasionally fractured the cryosphere, releasing enormous quantities of deep groundwater to the surface and carving huge outflow channels. Much of this water flowed into the northern hemisphere where it probably pooled to form large transient lakes or an ice covered ocean.

  1. ^ Hartmann, 2003, pp. 33–34.
  2. ^ a b Carr, M. H.; Head, J. W. (2010). "Geologic history of Mars". Earth and Planetary Science Letters. 294 (3–4): 185–203. Bibcode:2010E&PSL.294..185C. doi:10.1016/j.epsl.2009.06.042.
  3. ^ Tanaka, K. L. (1986). "The stratigraphy of Mars". Journal of Geophysical Research. 91 (B13): E139–E158. Bibcode:1986LPSC...17..139T. doi:10.1029/JB091iB13p0E139.
  4. ^ Hartmann, W. K.; Neukum, G. (2001). "Cratering Chronology and the Evolution of Mars". Space Science Reviews. 96: 165–194. Bibcode:2001SSRv...96..165H. doi:10.1023/A:1011945222010. S2CID 7216371.
  5. ^ Hartmann, W. K. (2005). "Martian cratering 8: Isochron refinement and the chronology of Mars". Icarus. 174 (2): 294–320. Bibcode:2005Icar..174..294H. doi:10.1016/j.icarus.2004.11.023.
  6. ^ Greeley, R.; Spudis, P. D. (1981). "Volcanism on Mars". Reviews of Geophysics. 19 (1): 13–41. Bibcode:1981RvGSP..19...13G. doi:10.1029/RG019i001p00013.
  7. ^ Werner, S. C. (2009). "The global martian volcanic evolutionary history". Icarus. 201 (1): 44–68. Bibcode:2009Icar..201...44W. doi:10.1016/j.icarus.2008.12.019.
  8. ^ Bibring, J.-P.; Langevin, Y.; Mustard, J. F.; Poulet, F.; Arvidson, R.; Gendrin, A.; Gondet, B.; Mangold, N.; Pinet, P.; Forget, F.; Berthe, M.; Bibring, J.-P.; Gendrin, A.; Gomez, C.; Gondet, B.; Jouglet, D.; Poulet, F.; Soufflot, A.; Vincendon, M.; Combes, M.; Drossart, P.; Encrenaz, T.; Fouchet, T.; Merchiorri, R.; Belluci, G.; Altieri, F.; Formisano, V.; Capaccioni, F.; Cerroni, P.; Coradini, A.; Fonti, S.; Korablev, O.; Kottsov, V.; Ignatiev, N.; Moroz, V.; Titov, D.; Zasova, L.; Loiseau, D.; Mangold, N.; Pinet, P.; Doute, S.; Schmitt, B.; Sotin, C.; Hauber, E.; Hoffmann, H.; Jaumann, R.; Keller, U.; Arvidson, R.; Mustard, J. F.; Duxbury, T.; Forget, F.; Neukum, G. (2006). "Global Mineralogical and Aqueous Mars History Derived from OMEGA/Mars Express Data". Science. 312 (5772): 400–404. Bibcode:2006Sci...312..400B. doi:10.1126/science.1122659. PMID 16627738.
  9. ^ Head, J.W.; Wilson, L. (2011). The Noachian-Hesperian Transition on Mars: Geological Evidence for a Punctuated Phase of Global Volcanism as a Key Driver in Climate and Atmospheric Evolution. 42nd Lunar and Planetary Science Conference (2011), Abstract #1214. http://www.lpi.usra.edu/meetings/lpsc2011/pdf/1214.pdf.
  10. ^ a b Barlow, N. G. (2010). "What we know about Mars from its impact craters". Geological Society of America Bulletin. 122 (5–6): 644–657. Bibcode:2010GSAB..122..644B. doi:10.1130/B30182.1.
  11. ^ Clifford, S. M. (1993). "A model for the hydrologic and climatic behavior of water on Mars". Journal of Geophysical Research. 98 (E6): 10973–11016. Bibcode:1993JGR....9810973C. doi:10.1029/93JE00225.