Hellas Planitia

Short description: 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| 2,300 km (1,400 mi)
Depth| 7,152 m (23,465 ft)
Topographic map of Hellas Planitia and its surroundings in the southern uplands, from the MOLA instrument of Mars Global Surveyor. The crater depth is 7,152 m (23,465 ft) below the standard topographic datum of Mars.[1]

Hellas Planitia /ˈhɛləs pləˈnɪʃiə/ is a plain located within the huge, roughly circular impact basin Hellas[lower-alpha 1] located in the southern hemisphere of the planet Mars.[3] Hellas is the fourth- or fifth-largest known impact crater in the Solar System. The basin floor is about 7,152 m (23,465 ft) deep, 3,000 m (9,800 ft) deeper than the Moon's 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.[3] It features the lowest point on Mars,[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 and the Noachis quadrangle.

## Contents

* 1 Description
* 2 Discovery and naming
* 3 Possible glaciers
* 4 Honeycomb terrain
* 5 Layers
* 6 In popular culture
* 7 See also
* 8 Notes
* 9 References
* 10 Further reading
* 11 External links

## Description

With a 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 is slightly larger (the Borealis Basin, if it proves to be an impact crater, is considerably larger). Hellas Planitia is thought to have been formed during the Late Heavy Bombardment period of the Solar System, approximately 4.1 to 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 and the bottom is over 9,000 m (30,000 ft). Despite being deeper than the Moon's 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 7,152 m (23,465 ft)[1] below the topographic datum of Mars explains the atmospheric pressure at the bottom: 12.4 mbar (1240 Pa or 0.18 psi) during winter, when the air is coldest and reaches its highest density.[lower-alpha 2] 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 of water, suggesting that the liquid phase 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 may be responsible for gully features in the crater.

Some of the low elevation outflow channels extend into Hellas from the volcanic Hadriacus Mons complex to the northeast, two of which Mars Orbiter Camera images show contain gullies: Dao Vallis and 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.[15][16][17] It and the somewhat smaller Isidis Planitia together are roughly antipodal to the Tharsis Bulge, with its enormous shield volcanoes, while Argyre Planitia is roughly antipodal to Elysium, 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.

File:Hellas and SP-A basins.pngElevation 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).

* 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 by telescope. Before Giovanni Schiaparelli gave it the name Hellas (which in Greek means Greece), it was known as Lockyer Land, having been named by Richard Anthony Proctor in 1867 in honor of Sir Joseph Norman Lockyer, an English astronomer who, using a 16 cm (6.3 in) refractor, produced "the first really truthful representation of the planet" (in the estimation of E. M. 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 (MRO) spacecraft's SHARAD radar sounder suggest that features called lobate debris aprons 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, 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 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. 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

* 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, 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. 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.
* In Planet-Size X-Men #1, the X-Men terraform 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
* Atmosphere of Mars e.g. pressure at floor of Hellas Planitia
* Dune
* Gale crater
* Geography of Mars
* Glaciers on Mars
* Groundwater on Mars
* List of plains on Mars
* Water on Mars

## Notes

1. ↑ Technically, Hellas is an 'albedo feature'.[2]
2. ↑ "... 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. ↑ 1.0 1.1 "Martian weather observation". Stanford University. http://www-star.stanford.edu/projects/mgs/sum/s0403210230.html. MGS radio science measured 11.50 mbar at 34.4° S 59.6° E −7152 meters
2. ↑ "Hellas". United States Geological Survey. http://planetarynames.wr.usgs.gov/Feature/2429.
3. ↑ 3.0 3.1 "Hellas Planitia". Gazetteer of Planetary Nomenclature. USGS Astrogeology Science Center. http://planetarynames.wr.usgs.gov/Feature/2432.
4. ↑ The part below zero datum, see Geography of Mars#Zero elevation
5. ↑ "Section 19-12". NASA. http://rst.gsfc.nasa.gov/Sect19/Sect19_12.html.
6. ↑ King, Hobart M.. "Highest and Lowest Points on Mars". https://geology.com/articles/highest-point-on-mars.shtml#mars-low-point.
7. ↑ Bleamaster, Leslie F. III; Crown, David A. (2010-03-19). "Geologic Map of MTM -40277, -45277, -40272, and -45272 Quadrangles, Eastern Hellas Planitia Region of Mars". https://pubs.usgs.gov/sim/3096/.
8. ↑ Schultz, Richard A.; Frey, Herbert V. (1990). "A new survey of multi-ring impact basins on Mars". Journal of Geophysical Research 95: 14175–14189. doi:10.1029/JB095iB09p14175. Bibcode: 1990JGR....9514175S. http://www.agu.org/pubs/crossref/1990/JB095iB09p14175.shtml. Retrieved 16 November 2008.
9. ↑ Acuña, M. H. (1999). "Global Distribution of Crustal Magnetization Discovered by the Mars Global Surveyor MAG/ER Experiment". Science 284 (5415): 790–793. doi:10.1126/science.284.5415.790. PMID 10221908. Bibcode: 1999Sci...284..790A. https://zenodo.org/record/1231157.
10. ↑ Branco, Hely C.; Miljkovic, Katarina; Plesa, Ana-Catalina (April 2024). "New Numerically Derived Scaling Relationships for Impact Basins on Mars" (in en). Journal of Geophysical Research: Planets 129 (4). doi:10.1029/2023JE008217. ISSN 2169-9097. Bibcode: 2024JGRE..12908217B.
11. ↑ Head, J.W.; Palumbo, A.M. (2018). "Impact cratering as a cause of climate change, surface alteration, and resurfacing". Meteoritics & Planetary Science 53, Nr4: 687–725. doi:10.1111/maps.13001. https://onlinelibrary.wiley.com/doi/pdf/10.1111/maps.13001.
12. ↑ Haberle, Robert M.; McKay, Christopher P.; Schaeffer, James; Cabrol, Nathalie A.; Grin, Edmon A.; Zent, Aaron P.; Quinn, Richard (October 25, 2001). "On the possibility of liquid water on present-day Mars". Journal of Geophysical Research 106 (EL0): 23,317–23,326. doi:10.1029/2000JE001360. Bibcode: 2001JGR...10623317H.
13. ↑ "Making a splash on Mars" (Press release). NASA. 29 June 2000. Archived from the original on 1 May 2017. Retrieved 12 July 2017.
14. ↑ Heldmann, Jennifer L. (2005). "Formation of Martian gullies by the action of liquid water flowing under current Martian environmental conditions". Journal of Geophysical Research 110 (E5): E05004. doi:10.1029/2004JE002261. Bibcode: 2005JGRE..110.5004H. – page 2, para 3: Martian Gullies Mars
15. ↑ Peterson, J. E. (March 1978). "Antipodal Effects of Major Basin-Forming Impacts on Mars". Lunar and Planetary Science IX: 885–886. Bibcode: 1978LPI.....9..885P.
16. ↑ Williams, D.A.; Greeley, R. (1991). "The Formation of Antipodal-Impact Terrains on Mars". Lunar and Planetary Science XXII: 1505–1506. http://www.lpi.usra.edu/meetings/lpsc1991/pdf/1748.pdf. Retrieved 2012-07-04.
17. ↑ Williams, D.A.; Greeley, R. (August 1994). "Assessment of Antipodal-Impact Terrains on Mars". Icarus 110 (2): 196–202. doi:10.1006/icar.1994.1116. Bibcode: 1994Icar..110..196W.
18. ↑ Sheehan, William (1996). The Planet Mars: A history of observation and discovery. Tucson, AZ: University of Arizona Press. Chapter 4. ISBN 9780816516414. http://www.uapress.arizona.edu/onlinebks/mars/chap04.htm. Retrieved 2021-02-19.
19. ↑ "PIA11433: Three craters". NASA. http://photojournal.jpl.nasa.gov/catalog/?IDNumber=pia11433.
20. ↑ 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". Science 311 (5759): 368–371. doi:10.1126/science.1120335. PMID 16424337. Bibcode: 2006Sci...311..368F. https://www.science.org/doi/10.1126/science.1120335. Retrieved 19 March 2025.
21. ↑ 21.0 21.1 Brough, S.; Hubbard, B.; Souness, C.; Grindrod, P. M.; Davis, J. (2015). "Landscapes of polyphase glaciation: eastern Hellas Planitia, Mars". Journal of Maps 12 (3): 530–542. doi:10.1080/17445647.2015.1047907. https://www.tandfonline.com/doi/full/10.1080/17445647.2015.1047907. Retrieved 19 March 2025.
22. ↑ 22.0 22.1 Bernhardt, H. (2016). "The honeycomb terrain on the Hellas basin floor, Mars: A case for salt or ice diapirism: Hellas honeycombs as salt / ice diapirs". J. Geophys. Res. 121 (4): 714–738. doi:10.1002/2016je005007. Bibcode: 2016JGRE..121..714B.
23. ↑ "HiRISE | to Great Depths (ESP_049330_1425)". http://www.uahirise.org/ESP_049330_1425.
24. ↑ 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.
25. ↑ 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. doi:10.1016/j.icarus.2016.11.016. Bibcode: 2017Icar..284..249W.

## Further reading

* Antoniadi, E.M. (July 1897). "The hourglass sea on Mars". Knowledge: 169–172.
* Sedimentary Geology of Mars. SEPM. 2012.
* Lockyer, J.N. (1863). "Observations on the planet Mars". Monthly Notices of the Royal Astronomical Society 23: 246. doi:10.1093/mnras/23.8.246. Bibcode: 1863MNRAS..23..246L.

## External links

* Ravenscroft, Peter (2000-08-16). "The Hellas of catastroph". http://www.spacedaily.com/news/mars-water-science-00i8.html.
* "Mars scrollable map". http://www.google.com/mars/#lat=-42.7&lon=70. – centered on Hellas
* Secosky, Jim. Martian ice (video lecture). 16th Annual International Mars Society Convention. Archived from the original on 2021-12-21 - via YouTube. * Cabrol, Nathalie. Lakes on Mars (video lecture). SETI Talks. Archived from the original on 2021-12-21 - via YouTube.

* v
* t
* e

Geography of Mars 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
* 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 and
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 and
plateaus|

* Acidalia Planitia
* Aeolis Palus
* Amazonis Planitia
* Arcadia Planitia
* 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

Canyons and
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
* Ma'adam
* 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 and 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
* Olympus Rupes
* Rupes Tenuis
* Angustus Labyrinthus
* Noctis Labyrinthus

Catenae and
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
* Eberswalde
* Eddie
* Ejriksson
* Emma Dean
* Endeavour
* Matijevic Hill
* Endurance
* Erebus
* Escalante
* Eudoxus
* Fenagh
* Fesenkov
* Firsoff
* Flammarion
* Flaugergues
* Focas
* Fontana
* Fournier
* Fram
* 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
* 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
* 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
* Wallace
* Wegener
* Weinbaum
* Wells
* Williams
* Winslow
* Wirtz
* Wislicenus
* Wright
* Yuty
* Zumba
* Zunil

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Original source: https://en.wikipedia.org/wiki/Hellas Planitia. Read more

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