# Hellas Planitia

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Planitia on Mars

Hellas Planitia Viking orbiter image mosaic of Hellas Planitia Location Hellas quadrangle, Mars Coordinates 42°24′S 70°30′E / 42.4°S 70.5°E / -42.4; 70.5 Diameter c. 2,300 km (1,400 mi) Impactor diameter c. 370 km Age c. 4 billion years

Topographic map of Hellas Planitia and its surroundings in the southern uplands, from the [MOLA](/source/Mars_Orbiter_Laser_Altimeter) instrument of *[Mars Global Surveyor](/source/Mars_Global_Surveyor)*. The crater depth is 7,152 m (23,465 ft) below the standard topographic [datum](/source/Datum_(geodesy)) of Mars.[1]

**Hellas Planitia** [/ˈhɛləs pləˈnɪʃiə/](https://en.wikipedia.org/wiki/Help:IPA/English) is a [plain](/source/Planitia) located within the huge, roughly circular [impact basin](/source/Impact_basin) **Hellas**[a] located in the southern [hemisphere](/source/Sphere) of the [planet](/source/Planet) [Mars](/source/Mars).[3] Hellas is the fourth or [fifth-largest known impact crater in the Solar System](/source/List_of_largest_craters_in_the_Solar_System). The basin floor is around 7,152 m (23,465 ft) deep, 3,000 m (9,800 ft) deeper than the Moon's [South Pole-Aitken basin](/source/South_Pole-Aitken_basin), and extends about 2,300 km (1,400 mi) east to west.[4][5] It is centered at [42°24′S 70°30′E / 42.4°S 70.5°E / -42.4; 70.5](https://geohack.toolforge.org/geohack.php?pagename=Hellas_Planitia&params=42.4_S_70.5_E_globe:mars_type:landmark).[3] It features the [lowest point on Mars](/source/Badwater_Crater),[6] serves as a known source of global dust storms, and may have contained lakes and glaciers.[7] Hellas Planitia spans the boundary between the [Hellas quadrangle](/source/Hellas_quadrangle) and the [Noachis quadrangle](/source/Noachis_quadrangle).

## Description

With a [diameter](/source/Diameter) of about 2,300 km (1,400 mi),[8] it is the largest unambiguous well-exposed impact structure on the planet; the obscured [Utopia Planitia](/source/Utopia_Planitia) is slightly larger (the [Borealis Basin](/source/North_Polar_Basin_(Mars)), if it proves to be an impact crater, is considerably larger). Hellas Planitia is thought to have been formed during the [Late Heavy Bombardment](/source/Late_Heavy_Bombardment) period of the [Solar System](/source/Solar_System), between 4.1-3.8 billion years ago, when a protoplanet or large asteroid, suggested to be around 370 kilometres (230 mi) in diameter, hit the surface.[9][10]

The altitude difference between the [rim](/source/Rim_(craters)) and the bottom is over 9,000 m (30,000 ft). Despite being deeper than the Moon's [South Pole-Aitken basin](/source/South_Pole-Aitken_basin), Hellas's rim peaks are significantly less prominent. This may be because large Martian impacts such as Hellas induced global hot rainfall and meltwater flows that degraded crater rims, including their own.[11] The crater's depth of around 7,152 m (23,465 ft)[1] below the topographic [datum](/source/Geodetic_datum) of Mars explains the atmospheric pressure at the bottom: 12.4 mbar (1,240 Pa or 0.18 psi) during winter, when the air is coldest and reaches its highest density.[b] This is 103% higher than the pressure at the topographical datum (610 Pa, or 6.1 mbar, or 0.09 psi) and above the [triple point](/source/Triple_point) of [water](/source/Water), suggesting that the [liquid phase](/source/Phase_(matter)) could be present under certain conditions of temperature, pressure, and dissolved salt content.[13] It has been theorized that a combination of glacial action and [explosive boiling](/source/Explosive_boiling) may be responsible for gully features in the crater.

Some of the low elevation outflow channels extend into Hellas from the volcanic [Hadriacus Mons](/source/Hadriacus_Mons) complex to the northeast, two of which [Mars Orbiter Camera](/source/Mars_Orbiter_Camera) images show contain gullies: [Dao Vallis](/source/Dao_Vallis) and [Reull Vallis](/source/Reull_Vallis). These gullies are also low enough for liquid water to be transient around Martian noon, if the temperature were to rise above 0° Celsius.[14]

Hellas Planitia is antipodal to [Alba Patera](/source/Alba_Mons).[15][16][17] It and the somewhat smaller [Isidis Planitia](/source/Isidis_Planitia) together are roughly [antipodal](/source/Antipodal_point) to the [Tharsis Bulge](/source/Tharsis_Bulge), with its enormous shield volcanoes, while [Argyre Planitia](/source/Argyre_Planitia) is roughly antipodal to [Elysium](/source/Elysium_(volcanic_province)), the other major uplifted region of shield volcanoes on Mars. Whether the shield volcanoes were caused by antipodal impacts like that which produced Hellas, or if it is mere coincidence, is unknown.

Elevation profiles along south to north transects across Mars's Hellas basin and the Moon's South Pole-Aitken basin, created with Lunar Quickmap and Mars Quickmap

		- MOLA map showing boundaries of Hellas Planitia and other regions

		- Geographic context of Hellas

		- This elevation map shows the surrounding elevated ring of ejecta

		- Apparent viscous flow features on the floor of Hellas, as seen by HiRISE.

		- Twisted terrain in Hellas Planitia (actually located in [Noachis quadrangle](/source/Noachis_quadrangle)).

		- Twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program

		- Twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program These twisted bands are also called "taffy pull" terrain.

## Discovery and naming

Due to its size and its light coloring, which contrasts with the rest of the planet, Hellas Planitia was one of the first Martian features discovered from [Earth](/source/Earth_(planet)) by [telescope](/source/Telescope). Before [Giovanni Schiaparelli](/source/Giovanni_Schiaparelli) gave it the name Hellas (which in Greek means *[Greece](/source/Greece)*), it was known as **Lockyer Land**, having been named by [Richard Proctor](/source/Richard_A._Proctor) in 1867 in honor of Sir [Joseph Lockyer](/source/Norman_Lockyer), an English astronomer who, using a 16 cm (6.3 in) [refractor](/source/Refracting_telescope), produced "the first really truthful representation of the planet" (in the estimation of [E. M. Antoniadi](/source/Eug%C3%A8ne_Michel_Antoniadi)).[18]

## Possible glaciers

Tongue-shaped glacier in Hellas Planitia. Ice may still exist there beneath an insulating layer of soil.

Close-up of glacier with a resolution of about 1 meter. The patterned ground is believed to be caused by the presence of ice.

Radar images by the [Mars Reconnaissance Orbiter](/source/Mars_Reconnaissance_Orbiter) (MRO) spacecraft's [SHARAD](/source/SHARAD) radar sounder suggest that features called [lobate debris aprons](/source/Lobate_debris_apron) in three craters in the eastern region of Hellas Planitia are actually glaciers of water ice lying buried beneath layers of dirt and rock.[19] The buried ice in these craters as measured by SHARAD is about 250 m (820 ft) thick on the upper crater and about 300 m (980 ft) and 450 m (1,480 ft) on the middle and lower levels respectively. Scientists believe that snow and ice accumulated on higher topography, flowed downhill, and is now protected from sublimation by a layer of rock debris and dust. Furrows and ridges on the surface were caused by deforming ice.

The shapes of many features in Hellas Planitia and other parts of Mars are strongly suggestive of [glaciers](/source/Glacier), as the surface looks as if movement has taken place. Advances in orbital and climatic modelling have supported earlier arguments that viscous flow features present in the mid-latitudes of Mars like Hellas Planitia are related to geologically recent ice ages.[20]

Select analysis of landforms in eastern Hellas Planitia[21] suggests that the detected ice deposits are remnants of a [complex history of glaciation](/source/Water_on_Mars#Ice_ages) and that the region has undergone at least two and possibly three, phases of glaciation. The presence of multiple overlapping glacial units indicates episodes of ice accumulation and flow, interrupted by periods of stagnation and burial under debris. Evidence recorded in the lobate debris aprons suggests that the region underwent a wider glacial period, while analysis of several glacier-like forms with several distinct structures indicative of flow and transportation of mass down-slope suggest additional subsequent more localised glaciation.[21]

## Honeycomb terrain

These relatively flat-lying "cells" appear to have concentric layers or bands, similar to a honeycomb. This *honeycomb terrain* was first discovered in the northwestern part of Hellas.[22] The geologic process responsible for creating these features remains unresolved.[23] Some calculations indicate that this formation may have been caused by ice moving up through the ground in this region. The ice layer would have been between 100 m and 1 km thick.[24][25][22] When one substance moves up through another denser substance, it is called a [diapir](/source/Diapir). So, it seems that large masses of ice have pushed up layers of rock into domes that were subsequently eroded. After erosion removed the top of the layered domes, circular features remained.

		- Honeycomb terrain, as seen by HiRISE under [HiWish program](/source/HiWish_program)

		- Close, color view of honeycomb terrain, as seen by HiRISE under HiWish program

		- Close view of honeycomb terrain, as seen by HiRISE under HiWish program

		- Close view of honeycomb terrain, as seen by HiRISE under HiWish program This enlargement shows material breaking up into blocks. Arrow indicates a cube-shaped block.

		- Twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program

		- Floor features in Hellas Planitia, as seen by HiRISE under HiWish program

		- Floor features in Hellas Planitia, as seen by HiRISE under HiWish program

## Layers

		- Layers in depression in crater, as seen by HiRISE under HiWish program A special type of sand ripple called [Transverse aeolian ridges](/source/Transverse_aeolian_ridges), TAR's are visible and labeled

		- Wide view of layers, as seen by HiRISE under HiWish program

		- Close view of layered deposit in crater, as seen by HiRISE under HiWish program

		- Layered formation, as seen by HiRISE under HiWish program

		- Close view of layers from previous image, as seen by HiRISE under HiWish program

## In popular culture

- Hellas Basin was a primary location in the 2017 video game *[Destiny 2](/source/Destiny_2)*. The location is part of the second game's *Warmind* downloadable content.

- It is also featured as a main location in the 2016 Bethesda video game reboot *[Doom](/source/Doom_(2016_video_game))*.

- In *Planet-Size X-Men #1*, the [X-Men](/source/X-Men) [terraform](/source/Terraforming) Mars, turning the basin into Lake Hellas and building the Lake Hellas Diplomatic Ring, where galactic ambassadors can meet within the Sol system.

## See also

- [Argyre Planitia](/source/Argyre_Planitia)

- [Atmosphere of Mars](/source/Atmosphere_of_Mars) e.g. pressure at floor of Hellas Planitia

- [Dune](/source/Dune)

- [Gale crater](/source/Gale_(crater))

- [Geography of Mars](/source/Geography_of_Mars)

- [Glaciers on Mars](/source/Glaciers_on_Mars)

- [Groundwater on Mars](/source/Groundwater_on_Mars)

- [List of plains on Mars](/source/List_of_plains_on_Mars)

- [Water on Mars](/source/Water_on_Mars)

## Notes

1. **[^](#cite_ref-3)** Technically, *Hellas* is an 'albedo feature'.[2]

1. **[^](#cite_ref-14)** "... the maximum surface pressure in the baseline simulation is only 12.4 mbar. This occurs in the bottom of the Hellas basin during northern summer."[12]

## References

1. ^ [***a***](#cite_ref-stanhellas_1-0) [***b***](#cite_ref-stanhellas_1-1) ["Martian weather observation"](https://web.archive.org/web/20080531235046/http://www-star.stanford.edu/projects/mgs/sum/s0403210230.html). [Mars Global Surveyor](/source/Mars_Global_Surveyor). Palo Alto, California: [Stanford University](/source/Stanford_University). Archived from [the original](http://www-star.stanford.edu/projects/mgs/sum/s0403210230.html) on 31 May 2008. MGS radio science measured 11.50 mbar at 34.4° S 59.6° E −7152 meters

1. **[^](#cite_ref-USGS_Hellas_2-0)** ["Hellas"](https://planetarynames.wr.usgs.gov/Feature/2429). [USGS Astrogeology Science Center](/source/USGS_Astrogeology_Science_Center). *Gazetteer of Planetary Nomenclature*. [United States Geological Survey](/source/United_States_Geological_Survey). Retrieved 10 March 2015.

1. ^ [***a***](#cite_ref-USGS_Hellas_Planitia_4-0) [***b***](#cite_ref-USGS_Hellas_Planitia_4-1) ["Hellas Planitia"](https://planetarynames.wr.usgs.gov/Feature/2432). *Gazetteer of Planetary Nomenclature*. [USGS Astrogeology Science Center](/source/USGS_Astrogeology_Science_Center). Retrieved 10 March 2015.

1. **[^](#cite_ref-Ref_5-0)** The part below zero datum, see [Geography of Mars#Zero elevation](/source/Geography_of_Mars#Zero_elevation)

1. **[^](#cite_ref-Ref_a_6-0)** ["Section 19-12"](https://web.archive.org/web/20041030132127/http://rst.gsfc.nasa.gov/Sect19/Sect19_12.html). [Goddard Space Flight Center](/source/Goddard_Space_Flight_Center). Remote sensing tutorial. NASA. Archived from [the original](https://rst.gsfc.nasa.gov/Sect19/Sect19_12.html) on 30 October 2004.

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1. **[^](#cite_ref-Acuna1999_10-0)** Acuña, M. H.; et al. (1999). ["Global Distribution of Crustal Magnetization Discovered by the Mars Global Surveyor MAG/ER Experiment"](https://zenodo.org/record/1231157). *Science*. **284** (5415): 790–793. [Bibcode](/source/Bibcode_(identifier)):[1999Sci...284..790A](https://ui.adsabs.harvard.edu/abs/1999Sci...284..790A). [doi](/source/Doi_(identifier)):[10.1126/science.284.5415.790](https://doi.org/10.1126%2Fscience.284.5415.790). [PMID](/source/PMID_(identifier)) [10221908](https://pubmed.ncbi.nlm.nih.gov/10221908).

1. **[^](#cite_ref-11)** Branco, Hely C.; Miljkovic, Katarina; Plesa, Ana-Catalina (April 2024). ["New Numerically Derived Scaling Relationships for Impact Basins on Mars"](https://doi.org/10.1029%2F2023JE008217). *Journal of Geophysical Research: Planets*. **129** (4). [Bibcode](/source/Bibcode_(identifier)):[2024JGRE..12908217B](https://ui.adsabs.harvard.edu/abs/2024JGRE..12908217B). [doi](/source/Doi_(identifier)):[10.1029/2023JE008217](https://doi.org/10.1029%2F2023JE008217). [ISSN](/source/ISSN_(identifier)) [2169-9097](https://search.worldcat.org/issn/2169-9097).

1. **[^](#cite_ref-12)** Head, J.W.; Palumbo, A.M. (2018). ["Impact cratering as a cause of climate change, surface alteration, and resurfacing"](https://onlinelibrary.wiley.com/doi/pdf/10.1111/maps.13001). *Meteoritics & Planetary Science*. 53, Nr4: 687–725. [doi](/source/Doi_(identifier)):[10.1111/maps.13001](https://doi.org/10.1111%2Fmaps.13001).

1. **[^](#cite_ref-Haberle_13-0)** Haberle, Robert M.; McKay, Christopher P.; Schaeffer, James; Cabrol, Nathalie A.; Grin, Edmon A.; Zent, Aaron P.; Quinn, Richard (25 October 2001). ["On the possibility of liquid water on present-day Mars"](https://doi.org/10.1029%2F2000JE001360). *Journal of Geophysical Research*. **106** (EL0): 23, 317–23, 326. [Bibcode](/source/Bibcode_(identifier)):[2001JGR...10623317H](https://ui.adsabs.harvard.edu/abs/2001JGR...10623317H). [doi](/source/Doi_(identifier)):[10.1029/2000JE001360](https://doi.org/10.1029%2F2000JE001360).

1. **[^](#cite_ref-Ref_c_15-0)** ["Making a splash on Mars"](https://web.archive.org/web/20170501032128/https://science.nasa.gov/science-news/science-at-nasa/2000/ast29jun_1m) (Press release). [NASA](/source/NASA). 29 June 2000. Archived from [the original](https://science.nasa.gov/science-news/science-at-nasa/2000/ast29jun_1m/) on 1 May 2017. Retrieved 12 July 2017.

1. **[^](#cite_ref-Heldmann2005_16-0)** Heldmann, Jennifer L.; et al. (2005). "Formation of Martian gullies by the action of liquid water flowing under current Martian environmental conditions". *Journal of Geophysical Research*. **110** (E5): E05004. [Bibcode](/source/Bibcode_(identifier)):[2005JGRE..110.5004H](https://ui.adsabs.harvard.edu/abs/2005JGRE..110.5004H). [CiteSeerX](/source/CiteSeerX_(identifier)) [10.1.1.596.4087](https://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.596.4087). [doi](/source/Doi_(identifier)):[10.1029/2004JE002261](https://doi.org/10.1029%2F2004JE002261). [S2CID](/source/S2CID_(identifier)) [1578727](https://api.semanticscholar.org/CorpusID:1578727). – page 2, para 3: Martian Gullies [Mars#References](/source/Mars#References)

1. **[^](#cite_ref-Peterson_17-0)** Peterson, J. E. (March 1978). "Antipodal Effects of Major Basin-Forming Impacts on Mars". *Lunar and Planetary Science*. **IX**: 885–886. [Bibcode](/source/Bibcode_(identifier)):[1978LPI.....9..885P](https://ui.adsabs.harvard.edu/abs/1978LPI.....9..885P).

1. **[^](#cite_ref-Williams_18-0)** Williams, D.A.; Greeley, R. (1991). ["The Formation of Antipodal-Impact Terrains on Mars"](http://www.lpi.usra.edu/meetings/lpsc1991/pdf/1748.pdf) (PDF). *Lunar and Planetary Science*. **XXII**: 1505–1506. Retrieved 4 July 2012.

1. **[^](#cite_ref-Williams2_19-0)** Williams, D.A.; Greeley, R. (August 1994). "Assessment of Antipodal-Impact Terrains on Mars". *[Icarus](/source/Icarus_(journal))*. **110** (2): 196–202. [Bibcode](/source/Bibcode_(identifier)):[1994Icar..110..196W](https://ui.adsabs.harvard.edu/abs/1994Icar..110..196W). [doi](/source/Doi_(identifier)):[10.1006/icar.1994.1116](https://doi.org/10.1006%2Ficar.1994.1116).

1. **[^](#cite_ref-William_20-0)** Sheehan, William (1996). [*The Planet Mars: A history of observation and discovery*](http://www.uapress.arizona.edu/onlinebks/mars/chap04.htm). Tucson, AZ: [University of Arizona Press](/source/University_of_Arizona_Press). Chapter 4. [ISBN](/source/ISBN_(identifier)) [9780816516414](https://en.wikipedia.org/wiki/Special:BookSources/9780816516414). Retrieved 19 February 2021.

1. **[^](#cite_ref-Nasa_21-0)** ["PIA11433: Three craters"](https://photojournal.jpl.nasa.gov/catalog/?IDNumber=pia11433). [NASA](/source/NASA). Retrieved 24 November 2008.

1. **[^](#cite_ref-Glacier1_22-0)** Forget, F.; Haberle, R. M.; Montmessin, F.; Levrard, B.; Head, J. W (20 January 2006). ["Formation of Glaciers on Mars by Atmospheric Precipitation at High Obliquity"](https://www.science.org/doi/10.1126/science.1120335). *Science*. **311** (5759): 368–371. [Bibcode](/source/Bibcode_(identifier)):[2006Sci...311..368F](https://ui.adsabs.harvard.edu/abs/2006Sci...311..368F). [doi](/source/Doi_(identifier)):[10.1126/science.1120335](https://doi.org/10.1126%2Fscience.1120335). [PMID](/source/PMID_(identifier)) [16424337](https://pubmed.ncbi.nlm.nih.gov/16424337). Retrieved 19 March 2025.

1. ^ [***a***](#cite_ref-Glacier2_23-0) [***b***](#cite_ref-Glacier2_23-1) Brough, S.; Hubbard, B.; Souness, C.; Grindrod, P. M.; Davis, J. (2015). ["Landscapes of polyphase glaciation: eastern Hellas Planitia, Mars"](https://www.tandfonline.com/doi/full/10.1080/17445647.2015.1047907). *Journal of Maps*. **12** (3): 530–542. [doi](/source/Doi_(identifier)):[10.1080/17445647.2015.1047907](https://doi.org/10.1080%2F17445647.2015.1047907). Retrieved 19 March 2025.

1. ^ [***a***](#cite_ref-ReferenceB_24-0) [***b***](#cite_ref-ReferenceB_24-1) Bernhardt, H.; et al. (2016). ["The honeycomb terrain on the Hellas basin floor, Mars: A case for salt or ice diapirism: Hellas honeycombs as salt / ice diapirs"](https://doi.org/10.1002%2F2016je005007). *J. Geophys. Res*. **121** (4): 714–738. [Bibcode](/source/Bibcode_(identifier)):[2016JGRE..121..714B](https://ui.adsabs.harvard.edu/abs/2016JGRE..121..714B). [doi](/source/Doi_(identifier)):[10.1002/2016je005007](https://doi.org/10.1002%2F2016je005007).

1. **[^](#cite_ref-25)** ["HiRISE | to Great Depths (ESP_049330_1425)"](http://www.uahirise.org/ESP_049330_1425).

1. **[^](#cite_ref-26)** Weiss, D.; Head, J. (2017). "Hydrology of the Hellas basin and the early Mars climate: Was the *honeycomb terrain* formed by salt or ice diapirism?". *Lunar and Planetary Science*. **XLVIII**: 1060.

1. **[^](#cite_ref-27)** Weiss, D.; Head, J. (2017). "Salt or ice diapirism origin for the *honeycomb terrain* in Hellas basin, Mars?: Implications for the early martian climate". *Icarus*. **284**: 249–263. [Bibcode](/source/Bibcode_(identifier)):[2017Icar..284..249W](https://ui.adsabs.harvard.edu/abs/2017Icar..284..249W). [doi](/source/Doi_(identifier)):[10.1016/j.icarus.2016.11.016](https://doi.org/10.1016%2Fj.icarus.2016.11.016).

## Further reading

- Antoniadi, E.M. (July 1897). "The hourglass sea on Mars". *Knowledge*. pp. 169–172.

- Grotzinger, J.; Milliken, R., eds. (2012). *Sedimentary Geology of Mars*. SEPM.

- Lockyer, J.N. (1863). ["Observations on the planet Mars"](https://doi.org/10.1093%2Fmnras%2F23.8.246). *[Monthly Notices of the Royal Astronomical Society](/source/Monthly_Notices_of_the_Royal_Astronomical_Society)* (abstract). **23**: 246. [Bibcode](/source/Bibcode_(identifier)):[1863MNRAS..23..246L](https://ui.adsabs.harvard.edu/abs/1863MNRAS..23..246L). [doi](/source/Doi_(identifier)):[10.1093/mnras/23.8.246](https://doi.org/10.1093%2Fmnras%2F23.8.246).

## External links

Wikimedia Commons has media related to [Hellas Planitia](https://commons.wikimedia.org/wiki/Category:Hellas_Planitia).

- Ravenscroft, Peter (16 August 2000). ["The Hellas of catastroph"](http://www.spacedaily.com/news/mars-water-science-00i8.html). *Space Daily*.

- ["Mars scrollable map"](http://www.google.com/mars/#lat=-42.7&lon=70). – centered on Hellas

- Secosky, Jim. [*Martian ice*](https://www.youtube.com/watch?v=_sUUKcZaTgA) (video lecture). 16th Annual International Mars Society Convention. [Archived](https://ghostarchive.org/varchive/youtube/20211221/_sUUKcZaTgA) from the original on 21 December 2021 – via YouTube.

- Cabrol, Nathalie. [*Lakes on Mars*](https://www.youtube.com/watch?v=DGBbke1wJRk) (video lecture). SETI Talks. [Archived](https://ghostarchive.org/varchive/youtube/20211221/DGBbke1wJRk) from the original on 21 December 2021 – via YouTube.

v t e Geography and geology of Mars Cartography Regions Abalos Undae Aspledon Undae Arabia Terra Cerberus Cydonia Eridania Lake Hyperboreae Undae Ogygis Undae Olympia Undae Planum Australe Planum Boreum Quadrangles Sinus Meridiani Siton Undae Tempe Terra Terra Cimmeria Terra Sabaea Tharsis Vastitas Borealis Quadrangles Aeolis Amazonis Amenthes Arabia Arcadia Argyre Casius Cebrenia Coprates Diacria Elysium Eridania Hellas Iapygia Ismenius Lacus Lunae Palus Mare Acidalium Mare Australe (South Pole) Mare Boreum (North Pole) Mare Tyrrhenum Margaritifer Sinus Memnonia Noachis Oxia Palus Phaethontis Phoenicis Lacus Sinus Sabaeus Syrtis Major Tharsis Thaumasia Geology Surface features Brain terrain Carbonates Chaos terrain Color Composition Concentric crater fill Dark slope streak Dichotomy Dune fields Hagal Nili Patera Fretted terrain Geysers Glaciers Groundwater Gullies Inverted relief Lakes Lava tubes Lineated valley fill (LVF) Lobate debris apron North Polar Basin Ocean hypothesis Ore resources Outflow channels Polar caps Ring mold craters Rootless cones Scalloped topography Seasonal flows Soil Spherules Surface Swiss cheese features Terrain softening Tholus Upper plains unit Valley networks Water discovery chronology Yardangs History Amazonian Hesperian Noachian Volcanology Observation history Canals (list) Classical albedo features Rocks observed Curiosity rover Bathurst Inlet Coronation Goulburn Hottah Jake Matijevic Link Rocknest Rocknest 3 Tintina Opportunity rover Bounce El Capitan Last Chance Sojourner rover Barnacle Bill Yogi Spirit rover Adirondack Home Plate Mimi Pot of Gold Viking Big Joe Other Face Monolith Meteorites found on Mars Block Island Heat Shield Mackinac Island Meridiani Planum Oileán Ruaidh Shelter Island Martian meteorites found on Earth Balsaltic Breccia Chassignites Nakhlites Shergottites Other List Topography Mountains, volcanoes (list by height) Acidalia Colles Alba Mons Anseris Mons Apollinaris Mons Ariadnes Colles Astapus Colles Ausonia Montes Avernus Colles Biblis Tholus Centauri Montes Charitum Montes Echus Montes Elysium Elysium Mons Albor Tholus Hecates Tholus Erebus Montes Galaxius Mons Hadriacus Mons Hellas Montes Jovis Tholus Libya Montes Mount Sharp Nereidum Montes Olympus Mons Phlegra Montes Syrtis Major Planum Tartarus Colles Tartarus Montes Tharsis Montes Ascraeus Pavonis Arsia Tharsis Tholus Tyrrhenus Mons Ulysses Tholus Uranius group Uranius Mons Ceraunius Tholus Uranius Tholus Plains, plateaus Acidalia Planitia Aeolis Palus Amazonis Planitia Arcadia Planitia Argentea Planum Argyre Planitia Chryse Planitia Daedalia Planum Elysium Planitia Eridania Planitia Hellas Planitia Hesperia Planum Icaria Planum Isidis Planitia Lunae Planum Meridiani Planum Oxia Planum Planum Australe Planum Boreum Syria Planum Syrtis Major Planum Utopia Planitia Eden Patera Orcus Patera Peneus Patera Pityusa Patera Siloe Patera Canyons, valleys Aram Chaos Arsia Chasmata Aromatum Chaos Atlantis Chaos Aureum Chaos Candor Chasma Chasma Boreale Coprates Chasma Echus Chasma Eos Chaos Eos Chasma Galaxias Chaos Ganges Chasma Gorgonum Chaos Hebes Chasma Hydaspis Chaos Hydraotes Chaos Iani Chaos Ister Chaos Ius Chasma Juventae Chasma Melas Chasma Ophir Chasma Tithonium Chasma List of valles Apsus Ares Arnus Asopus Athabasca Auqakuh Bahram Buvinda Dao Enipeus Frento Granicus Green Valley Harmakhis Hebrus Her Desher Hrad Huo Hsing Hypanis Iberus Indus Ituxi Kasei Labou Ladon Lethe Licus Louros Maʼadim Mad Maja Mamers Mangala Marineris Labes Marte Maumee Mawrth Minio Naktong Nanedi Niger Nirgal Padus Paraná Patapsco Peace Rahway Ravi Reull Sabis Sabrina Samara Scamander Shalbatana Simud Stura Tader Tinia Tinjar Tiu Tyras Uzboi ULM Vedra Verde Warrego Fossae, mensae, rupes, labyrinthi Amenthes Fossae Ceraunius Fossae Cerberus Fossae Coloe Fossae Cyane Fossae Elysium Fossae Hephaestus Fossae Icaria Fossae Labeatis Fossae Mangala Fossa Mareotis Fossae Medusae Fossae Memnonia Fossae Nili Fossae Olympica Fossae Oti Fossae Sirenum Fossae Tantalus Fossae Tempe Fossae Tithonium Fossae Tractus Fossae Ulysses Fossae Aeolis Mensae Ausonia Mensa Capri Mensa Cydonia Mensae Deuteronilus Mensae Ganges Mensa Nilosyrtis Mensae Protonilus Mensae Sacra Mensa Claritas Rupes Nilokeras Scopulus Olympus Rupes Rupes Tenuis Angustus Labyrinthus Noctis Labyrinthus Catenae, craters Artynia Catena Tithoniae Catenae Tractus Catena Adams Agassiz Airy Airy-0 Aniak Antoniadi Arandas Argo Arkhangelsky Arrhenius Asimov Bacolor Bakhuysen Baldet Baltisk Bamberg Barabashov Barnard Beagle Becquerel Beer Belz Bernard Bianchini Boeddicker Bok Bond Bonestell Bonneville Brashear Briault Burroughs Burton Campbell Canso Cassini Caxias Cerulli Chafe Chapais Chincoteague Chryse Alien Clark Coblentz Columbus Copernicus Corby Crewe Crivitz Crommelin Cruls Curie Da Vinci Danielson Darwin Davies Dawes Dejnev Denning Dilly Dinorwic Douglass Dromore Du Martheray Eagle (Acidalia Planitia) Eagle (Meridiani Planum) Eberswalde Eddie Ejriksson Emma Dean Endeavour Matijevic Hill Endurance Erebus Escalante Eudoxus Fenagh Fesenkov Firsoff Flammarion Flaugergues Focas Fontana Fournier Fram Freedom Galdakao Gale Galle Garni Gasa Gilbert Gill Gledhill Gold Graff Green Grindavik Gusev Apollo 1 Hills Chaffee Grissom White Columbia Hills Husband McCool Sleepy Hollow Hadley Haldane Hale Halley Hargraves Hartwig Heaviside Heimdal Heinlein Helmholtz Henry Herschel Hipparchus Holden Holmes Hooke Huggins Hussey Hutton Huxley Huygens Iazu Ibragimov Inuvik Janssen Jarry-Desloges Jeans Jezero Jezža Joly Jones Kaiser Keeler Kepler Kinkora Kipini Knobel Koga Korolev Kufra Kuiper Kunowsky Lambert Lamont Lampland Lassell Lau Le Verrier Li Fan Liais Lipik Liu Hsin Llanesco Lockyer Lod Lohse Lomonosov Louth Lowell Lyell Lyot Mädler Magelhaens Maggini Main Mandora Maraldi Mariner Marth Martz Masursky Maunder McLaughlin McMurdo Mellish Mendel Mie Milankovic Millochau Mitchel Miyamoto Mohawk Mojave Molesworth Montevallo Moreux Müller Nansen Nereus Newton Nhill Nicholson Niesten Nipigon Onon Orson Welles Oudemans Palana Pangboche Pasteur Penticton Perepelkin Peridier Persbo Pettit Phillips Pickering Playfair Pollack Poona Porter Porth Priestley Proctor Ptolemaeus Puńsk Quenisset Rabe Radau Rahe Rayleigh Redi Renaudot Reuyl Reynolds Richardson Ritchey Robert Sharp Roddenberry Ross Rossby Rudaux Russell Rutherford Sagan Saheki Santa Maria Schaeberle Schiaparelli Schmidt Secchi Semeykin Sharonov Sibu Sinton Sitka Sklodowska Slipher Smith South Spallanzani Srīpur Steno Stokes Stoney Suess Suzhi Tarsus Taytay Teisserenc de Bort Terby Thila Thira Tikhonravov Tikhov Timbuktu Tombaugh Tooting Trouvelot Troy Trud Trumpler Tugaske Tycho Brahe Tyndall Udzha Vernal Very Victoria Cape Verde Vinogradov Vinogradsky Virrat Vishniac Vogel Von Kármán Vostok Wallace Wegener Weinbaum Wells Williams Winslow Wirtz Wislicenus Wright Yuty Zumba Zunil

[Portals](https://en.wikipedia.org/wiki/Wikipedia:Contents/Portals):
- [Astronomy](https://en.wikipedia.org/wiki/Portal:Astronomy)
- [Stars](https://en.wikipedia.org/wiki/Portal:Stars)
- [Spaceflight](https://en.wikipedia.org/wiki/Portal:Spaceflight)
- [Outer space](https://en.wikipedia.org/wiki/Portal:Outer_space)
- [Solar System](https://en.wikipedia.org/wiki/Portal:Solar_System)

Authority control databases: National United States Israel

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Adapted from the Wikipedia article [Hellas Planitia](https://en.wikipedia.org/wiki/Hellas_Planitia) by Wikipedia contributors ([contributor history](https://en.wikipedia.org/wiki/Hellas_Planitia?action=history)). Available under [Creative Commons Attribution-ShareAlike 4.0 International](https://creativecommons.org/licenses/by-sa/4.0/). Changes may have been made.