178:
ejecta and rims should stand above upland elevations. The rims and ejecta blankets of the lowland impact craters are still much below the upland areas. There are also areas in the lowlands that are outside any of the impact basins, these areas must be overlain by multiple ejecta blankets and should stand at elevations similar to the original planetary surface. That clearly is not the case either. One approach explaining the absence of ejecta blankets infers that no ejecta was ever present. Absence of ejecta could be caused by a large impactor scattering the ejecta into outer space. Another approach proposed the formation of the dichotomy by cooling at depth and crustal loading by later volcanism. The multiple-impact hypothesis is also statistically unfavorable, it is unlikely that multiple impacts basins occur and overlap primarily in the northern hemisphere.
20:
150:
believed to be involved as cells or plumes. Since endogenic processes of Earth have yet to be completely understood, studying of similar processes on Mars is very difficult. The dichotomy could be created at the time of the creation of the
Martian core. The roughly circular shape of the lowland could then be attributed to plume-like first-order overturn which could occur in the process of rapid core formation. There is evidence for internally driven tectonic events in the vicinity of the lowland area that clearly occurred at the end of the
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but could not explain the absence of volcanoes. Also, the mega-impact could have scattered a large portion of the debris into outer space and across the southern hemisphere. Geologic evidence of the debris would provide very convincing support for this hypothesis. A 2008 study provided additional research towards the single giant impact theory in the northern hemisphere. In the past tracing of the impact boundaries was complicated by the presence of the
118:. However, most estimations of the shape of the lowlands area produce a shape that in places dramatically deviates from the circular shape. Additional processes could create those deviations from circularity. Also, if the proposed Borealis basin is a depression created by an impact, it would be the largest impact crater known in the Solar System. An object that large could have hit Mars sometime during the process of the Solar System accretion.
98:
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dramatic. Three major hypotheses have been proposed for the origin of the crustal dichotomy: endogenic (by mantle processes), single impact, or multiple impact. Both impact-related hypotheses involve processes that could have occurred before the end of the primordial bombardment, implying that the crustal dichotomy has its origins early in the history of Mars.
131:
dichotomy observed. This may have also triggered the magnetic field of the planet. The discovery of twelve volcanic alignments lends evidence to this new hypothesis. Initially, the estimated size of the impacting body required for this scenario was Moon-sized, but more recent research favour a smaller, 500-750 km-radius projectile.
156:
A 2005 study suggests that degree-1 mantle convection could have created the dichotomy. Degree-1 mantle convection is a convective process in which one hemisphere is dominated by an upwelling, while the other hemisphere is downwelling. Some of the evidence is the abundance of extensive fracturing and
121:
It is expected that an impact of such magnitude would have produced an ejecta blanket that should be found in areas around the lowland and generate enough heat to form volcanoes. However, if the impact occurred around 4.5 Ga (billion years ago), erosion could explain the absence of the ejecta blanket
149:
could have been active on Mars early in the planet's history. Large-scale redistribution of lithospheric crustal material is known to be caused by plate tectonic processes on Earth. Even though it is still not entirely clear how mantle processes affect plate tectonics on Earth, mantle convection is
198:
More visibly, dust storms originate in the
Southern hemisphere far more often than in the North. High Northern dust content tends to occur after exceptional Southern storms escalate into global dust storms. As a consequence, opacity (tau) is often higher in the Southern hemisphere. The effect of
177:
The multiple impact hypothesis is supported by correlation of segments of the dichotomy with the rims of several large impact basins. But there are large parts of the
Borealis Basin outside the rims of those impact basins. If the Martian lowlands were formed by the multiple basins then their inner
165:
age. A counter argument to the endogenic hypothesis is the possibility of those tectonic events occurring in the
Borealis Basin due to the post-impact weakening of the crust. In order to further support the endogenic origin hypothesis geologic evidence of faulting and flexing of the crust prior to
130:
However, this hypothesis has been countered by a new hypothesis of a giant impact to the south pole of Mars with a large object that melted the southern hemisphere of Mars, which, after recrystallisation, forms a thicker crust relative to the northern hemisphere and thus gives rise to the crustal
235:
of Mars is offset from symmetry about its equator. When combined with the greater seasonal range of the
Southern hemisphere (see above), this results in "the striking north-south hemispherical asymmetries of the atmospheric and residual ice cap inventories of Mars water", "as well as the current
126:
volcanic rise. The
Tharsis volcanic rise buried part of the proposed dichotomy boundary under 30 km of basalt. The researchers at MIT and Jet Propulsion Lab at CIT have been able to use gravity and topography of Mars to constrain the location of the dichotomy beneath the Tharsis rise, thus
87:
The northern lowlands comprise about one-third of the surface of Mars and are relatively flat, with as many impact craters as the southern hemisphere. The other two-thirds of the
Martian surface are the highlands of the southern hemisphere. The difference in elevation between the hemispheres is
34:, between the Southern and the Northern hemispheres. The two hemispheres' geography differ in elevation by 1 to 3 km. The average thickness of the Martian crust is 45 km, with 32 km in the northern lowlands region, and 58 km in the southern highlands.
1400:
Golabek, Gregor J.; Keller, Tobias; Gerya, Taras V.; Zhu, Guizhi; Tackley, Paul J.; Connolly, James A.D. (September 2011). "Origin of the martian dichotomy and
Tharsis from a giant impact causing massive magmatism".
79:
transitional zone, the dichotomy boundary is characterized by an escarpment with a local relief of about 2 km, and interconnected NW-SE-trending closed depressions at the foot of the dichotomy probably related to
127:
creating an elliptical model of the dichotomy boundary. The elliptical shape of the
Borealis basin contributed to the northern single impact hypothesis as a re-edition of the original theory published in 1984.
826:
Baker, D.; et al. (2010). "Flow patterns of lobate debris aprons and lineated valley fill north of
Ismeniae Fossae, Mars: Evidence for extensive mid-latitude glaciation in the Late Amazonian".
219:. This results in one hemisphere, the Southern, receiving more sunlight in summer and less in winter, and thus more extreme temperatures, than the Northern. When combined with Mars' much higher
308:
253:
495:
Greeley, R. and J. Guest. 1987. Geological map of the eastern equatorial region of Mars, scale 1:15,000,000. U. S. Geol. Ser. Misc. Invest. Map I-802-B, Reston, Virginia
1600:
O'Rourke, Joseph G.; Korenaga, Jun (2012-11-01). "Terrestrial planet evolution in the stagnant-lid regime: Size effects and the formation of self-destabilizing crust".
281:
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north-south asymmetry of the seasonal ice cap albedos". The atmosphere of Mars is currently "a nonlinear pump of water into the northern hemisphere of Mars."
250:
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Plaut, J. et al. 2008. Radar Evidence for Ice in Lobate Debris Aprons in the Mid-Northern Latitudes of Mars. Lunar and Planetary Science XXXIX. 2290.pdf
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Andrews-Hanna, Jeffrey C.; Zuber, Maria T.; Banerdt, W. Bruce (2008-06-26). "The Borealis basin and the origin of the martian crustal dichotomy".
305:
332:
over the image to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative
269:
1730:
Clancy, R. T.; Grossman, A. W.; et al. (Jul 1996). "Water Vapor Saturation at Low Altitudes around Mars Aphelion: A Key to Mars Climate?".
309:
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1553:"Towards scaling laws for subduction initiation on terrestrial planets: constraints from two-dimensional steady-state convection simulations"
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258:
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Andrews-Hanna, Jeffrey C.; Zuber, Maria T.; Banerdt, W. Bruce (2008). "The Borealis basin and the origin of the martian crustal dichotomy".
261:
1428:
Ballantyne, Harry A.; Jutzi, Martin; Golabek, Gregor J.; Mishra, Lokesh; Cheng, Kar Wai; Rozel, Antoine B.; Tackley, Paul J. (March 2023).
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67:. All three regions have been studied extensively because they contain landforms believed to have been produced by the movement of ice or
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304:
303:
300:
280:
260:
249:
298:
272:
791:
Leone, Giovanni (2016-01-01). "Alignments of volcanic features in the southern hemisphere of Mars produced by migrating mantle plumes".
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varies significantly between Northern and Southern hemispheres, both for reasons related and unrelated to the geographic dichotomy.
389:
2019:
1092:
Marinova, Margarita M.; Aharonson, Oded; Asphaug, Erik (2008-06-26). "Mega-impact formation of the Mars hemispheric dichotomy".
275:
274:
251:
2089:
745:
Leverington, David W. (2011-09-15). "A volcanic origin for the outflow channels of Mars: Key evidence and major implications".
114:
A single mega-impact would produce a very large, circular depression in the crust. The proposed depression has been named the
41:. It contains mesas, knobs, and flat-floored valleys having walls about a mile high. Around many of the mesas and knobs are
2228:
2213:
900:
645:
585:
556:
2687:
283:
1944:
661:
Leone, Giovanni (2014-05-01). "A network of lava tubes as the origin of Labyrinthus Noctis and Valles Marineris on Mars".
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2029:
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compared to Earth, and far thinner atmosphere in general, Southern winters and summers are wider ranging than on Earth.
2682:
1697:
2311:
1353:"Three-dimensional simulations of the southern polar giant impact hypothesis for the origin of the Martian dichotomy"
1304:"Three-dimensional simulations of the southern polar giant impact hypothesis for the origin of the Martian dichotomy"
1255:"Three-dimensional simulations of the southern polar giant impact hypothesis for the origin of the Martian dichotomy"
1210:
Wilhelms, Don E.; Squyres, Steven W. (1984-05-10). "The martian hemispheric dichotomy may be due to a giant impact".
869:
151:
1653:
Frey, H.; Schultz, R.A. (1988). "Large impact basins and the mega-impact origin for the crustal dichotomy of Mars".
1964:
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2004:
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The boundary between the two regions is quite complex in places. One distinctive type of topography is called
2417:
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1914:
363:
2788:
2579:
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2283:
2169:
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1006:
McGill, G. E.; Squyres, S. W (1991). "Origin of the martian crustal dichotomy: Evaluating hypotheses".
2699:
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2206:
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Many large valleys formed by the lava erupted from the volcanoes of Mars cut through the dichotomy.
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2186:
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1949:
19:
1999:
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2389:
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1978:
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higher dust content is to increase absorption of sunlight, increasing atmospheric temperature.
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2248:
2196:
2191:
2174:
2051:
2036:
926:"Geologic map of the Terra Cimmeria-Nepenthes Mensae transitional zone, Mars – 1:1.45Million"
81:
1351:
Leone, Giovanni; Tackley, Paul J.; Gerya, Taras V.; May, Dave A.; Zhu, Guizhi (2014-12-28).
1302:
Leone, Giovanni; Tackley, Paul J.; Gerya, Taras V.; May, Dave A.; Zhu, Guizhi (2014-12-28).
1253:
Leone, Giovanni; Tackley, Paul J.; Gerya, Taras V.; May, Dave A.; Zhu, Guizhi (2014-12-28).
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2084:
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1512:"Degree-1 convection in the Martian mantle and the origin of the hemispheric dichotomy"
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717:
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942:
698:"Volcanic rilles, streamlined islands, and the origin of outflow channels on Mars"
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2014:
2009:
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1904:
1879:
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1429:
1414:
959:"Impact constraints on, and a chronology for, major events in early Mars history"
847:
439:
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68:
38:
925:
2652:
1974:
1929:
1884:
442: – Scientific study of the surface, crust, and interior of the planet Mars
72:
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892:
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1994:
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1180:
1121:
992:
731:
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533:
2721:
2716:
2657:
2589:
2569:
2233:
1989:
1934:
1874:
1751:
1720:
De Pateris, I., Lissauer, J. Planetary Sciences Cambridge University Press
1188:
1129:
1070:
634:
448: – Persistent body of ice that is moving downhill under its own weight
46:
861:
2466:
2461:
1924:
1771:
1536:
1511:
1377:
1328:
1279:
983:
958:
722:
697:
1172:
1113:
1062:
597:
Squyres, S (1978). "Martian fretted terrain: Flow of erosional debris".
549:
Imagery & Creativity: Ethnoaesthetics and Art Worlds in the Americas
2574:
2559:
1894:
1824:
208:
1496:
1430:"Investigating the feasibility of an impact-induced Martian Dichotomy"
169:
However, the lack of plate tectonics on Mars weakens this hypothesis.
2726:
2662:
2296:
2159:
1231:
371:
333:
321:
162:
105:
of Mars with 20× elevation exaggeration showing the Martian dichotomy
1984:
580:
Carr, M. 2006. The Surface of Mars. Cambridge University Press.
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1352:
1303:
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367:
212:
158:
1614:
1939:
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123:
97:
316:
1690:
Mars: An Introduction to its Interior, Surface, and Atmosphere
216:
1729:
1427:
1807:
421: – Delineation and characterization of Martian regions
55:
The Martian dichotomy boundary includes the regions called
27:
1767:
1150:
1040:
1091:
466: – Fretted terrain in the Casius quadrangle on Mars
1776:
436: – Surface feature common to certain areas of Mars
423:
Pages displaying short descriptions of redirect targets
2786:
1551:
Wong, Teresa; Solomatov, Viatcheslav S (2015-07-02).
1399:
346:. Whites and browns indicate the highest elevations (
1599:
1350:
1301:
1252:
226:
882:
633:
358:; greens and blues are lower elevations (down to
166:the end of the primordial bombardment is needed.
71:questioned as formed by volcanic erosion. In the
2810:
1209:
478: – Study of past and present water on Mars
248:
885:Encyclopedia of Planetary Landforms - Springer
793:Journal of Volcanology and Geothermal Research
663:Journal of Volcanology and Geothermal Research
202:
134:
1792:
1550:
1005:
172:
1509:
923:
207:The spin axis of Mars, as with many bodies,
1652:
883:Hargitai, Henrik; Kereszturi, Ákos (2015).
744:
695:
109:
1799:
1785:
1613:
1576:
1535:
1510:Roberts, James H.; Zhong, Shijie (2006).
1455:
1445:
1376:
1327:
1278:
982:
941:
721:
211:over millions of years. At present, the
963:Journal of Geophysical Research: Planets
702:Journal of Geophysical Research: Planets
244:
95:
18:
1557:Progress in Earth and Planetary Science
786:
784:
631:
596:
546:
239:
2811:
1687:
454: – Extraterrestrial bodies of ice
1780:
1470:
862:"HiRISE - Glacier? (ESP_018857_2225)"
825:
790:
660:
504:
956:
781:
696:Leverington, David W. (2004-10-01).
507:"Mars Fretted and chaotic terrains"
460: – Geological features on Mars
13:
30:is a sharp contrast, known as the
14:
2830:
1761:
632:Kieffer, Hugh H. (October 1992).
2796:
2769:
2758:
2757:
872:from the original on 2017-05-30.
813:10.1016/j.jvolgeores.2015.10.028
683:10.1016/j.jvolgeores.2014.01.011
315:
227:Hadley circulation and volatiles
26:The most conspicuous feature of
16:Geomorphological feature of Mars
1723:
1714:
1681:
1646:
1593:
1544:
1516:Journal of Geophysical Research
1503:
1477:Journal of Geophysical Research
1464:
1421:
1393:
1344:
1295:
1246:
1203:
1144:
1085:
1034:
999:
950:
917:
876:
854:
819:
738:
350:); followed by pinks and reds (
96:
1692:. Cambridge University Press.
767:10.1016/j.geomorph.2011.05.022
689:
654:
625:
590:
574:
565:
540:
498:
489:
419:Areography (geography of Mars)
193:
1:
943:10.1080/17445647.2023.2227205
547:Whitten, Dorothea S. (1993).
483:
181:
2214:Recurring slope lineae (RSL)
1632:10.1016/j.icarus.2012.10.015
1457:10.1016/j.icarus.2022.115395
1415:10.1016/j.icarus.2011.06.012
1357:Geophysical Research Letters
1308:Geophysical Research Letters
1259:Geophysical Research Letters
1028:10.1016/0019-1035(91)90221-e
924:García-Arnay, Ángel (2023).
848:10.1016/j.icarus.2009.11.017
619:10.1016/0019-1035(78)90048-9
338:Mars Orbiter Laser Altimeter
7:
2648:Inspiration Mars Foundation
411:
215:nearly coincide with Mars'
203:Precession of the equinoxes
135:Endogenic origin hypothesis
45:that have been shown to be
10:
2835:
2683:Artificial objects on Mars
957:Frey, H. V. (2006-08-01).
173:Multiple impact hypothesis
138:
2752:
2700:List of films set on Mars
2675:
2626:
2608:
2552:
2543:
2523:
2515:C/2013 A1 (Siding Spring)
2507:
2428:
2380:
2333:
2324:
2312:Classical albedo features
2282:
2070:
1963:
1865:
1832:
1823:
1814:
1578:10.1186/s40645-015-0041-x
1473:"Martian plate tectonics"
893:10.1007/978-1-4614-3134-3
336:, based on data from the
326:global topography of Mars
157:igneous activity of late
91:
2618:List of missions to Mars
1806:
152:early bombardment phase.
147:plate tectonic processes
110:Single impact hypothesis
2776:Solar System portal
1675:10.1029/gl015i003p00229
534:10.1029/jb078i020p04073
217:aphelion and perihelion
2390:Solar eclipses on Mars
2249:"Swiss cheese" feature
2105:Concentric crater fill
1752:10.1006/icar.1996.0108
430: – Mensae on Mars
404:
106:
23:
472: – Martian plain
322:Interactive image map
313:
101:
82:extensional tectonics
22:
2590:Permanent settlement
1537:10.1029/2005je002668
1378:10.1002/2014GL062261
1363:(24): 2014GL062261.
1329:10.1002/2014GL062261
1314:(24): 2014GL062261.
1280:10.1002/2014GL062261
1265:(24): 2014GL062261.
984:10.1029/2005JE002449
723:10.1029/2004JE002311
343:Mars Global Surveyor
240:Interactive Mars map
145:It is believed that
43:lobate debris aprons
2732:Timekeeping on Mars
2409:Planetary transits
2394:Satellite transits
2307:Observation history
2155:Lobate debris apron
1744:1996Icar..122...36C
1688:Barlow, N. (2008).
1667:1988GeoRL..15..229F
1624:2012Icar..221.1043O
1569:2015PEPS....2...18W
1528:2006JGRE..111.6013R
1489:1994JGR....99.5639S
1369:2014GeoRL..41.8736L
1320:2014GeoRL..41.8736L
1271:2014GeoRL..41.8736L
1224:1984Natur.309..138W
1173:10.1038/nature07011
1165:2008Natur.453.1212A
1159:(7199): 1212–1215.
1114:10.1038/nature07070
1106:2008Natur.453.1216M
1100:(7199): 1216–1219.
1063:10.1038/nature07011
1055:2008Natur.453.1212A
1049:(7199): 1212–1215.
1020:1991Icar...93..386M
975:2006JGRE..111.8S91F
840:2010Icar..207..186B
805:2016JVGR..309...78L
759:2011Geomo.132...51L
714:2004JGRE..10910011L
675:2014JVGR..277....1L
611:1978Icar...34..600S
526:1973JGR....78.4073S
458:Lobate debris apron
428:Deuteronilus Mensae
57:Deuteronilus Mensae
1655:Geophys. Res. Lett
405:
233:Hadley circulation
188:atmosphere of Mars
107:
24:
2784:
2783:
2737:Sol (day on Mars)
2705:Martian scientist
2688:Memorials on Mars
2671:
2670:
2642:The Case for Mars
2539:
2538:
2320:
2319:
2254:Terrain softening
2219:Ring mold craters
2187:North Polar Basin
2110:Dark slope streak
1955:Vastitas Borealis
1852:Dust devil tracks
1497:10.1029/94JE00216
1218:(5964): 138–140.
902:978-1-4614-3133-6
647:978-0-8165-1257-7
586:978-0-521-87201-0
558:978-0-8165-1247-8
520:(20): 4073–4083.
505:Sharp, R (1973).
470:Protonilus Mensae
464:Nilosyrtis Mensae
390:Mars Memorial map
348:+12 to +8 km
141:Tectonics of Mars
65:Nilosyrtis Mensae
61:Protonilus Mensae
32:Martian dichotomy
2826:
2801:
2800:
2799:
2792:
2774:
2773:
2772:
2761:
2760:
2635:The Mars Project
2550:
2549:
2498:
2488:
2478:
2456:
2454:
2453:
2331:
2330:
2192:Ocean hypothesis
2042:Outflow channels
1830:
1829:
1801:
1794:
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1777:
1756:
1755:
1727:
1721:
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1608:(2): 1043–1060.
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452:Glaciers on Mars
424:
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352:+8 to +3 km
349:
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247:
100:
77:Nepenthes Mensae
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2370:Voltaire crater
2348:Stickney crater
2316:
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2120:Fretted terrain
2066:
1966:
1959:
1920:Sinus Meridiani
1905:Planum Australe
1880:Cerberus (Mars)
1861:
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1817:Outline of Mars
1810:
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514:J. Geophys. Res
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440:Geology of Mars
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2229:Seasonal flows
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2224:Rootless cones
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2059:
2054:
2052:Valley network
2049:
2044:
2039:
2037:Observed rocks
2034:
2033:
2032:
2022:
2017:
2012:
2007:
2002:
1997:
1992:
1987:
1982:
1971:
1969:
1961:
1960:
1958:
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1950:Ultimi Scopuli
1947:
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1930:Terra Cimmeria
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1763:
1762:External links
1760:
1758:
1757:
1722:
1713:
1699:978-1107644878
1698:
1680:
1661:(3): 229–232.
1645:
1592:
1543:
1522:(E6): E06013.
1502:
1471:Sleep (1994).
1463:
1420:
1409:(1): 346–357.
1392:
1343:
1294:
1245:
1202:
1143:
1084:
1033:
1014:(2): 386–393.
998:
969:(E8): E08S91.
949:
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875:
853:
834:(1): 186–209.
818:
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753:(3–4): 51–75.
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73:Terra Cimmeria
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2585:Human mission
2583:
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2580:Sample return
2578:
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2090:Chaos terrain
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2080:Brain terrain
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1995:Chaos terrain
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1910:Planum Boreum
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1900:Olympia Undae
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1890:Eridania Lake
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748:
747:Geomorphology
741:
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729:
724:
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684:
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476:Water on Mars
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377:
376:Polar regions
373:
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354:); yellow is
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66:
62:
58:
53:
50:
48:
47:rock glaciers
44:
40:
35:
33:
29:
21:
2803:Solar System
2722:Life on Mars
2717:Flag of Mars
2658:Mars Society
2640:
2633:
2600:Terraforming
2595:Colonization
2365:Swift crater
2207:polar wander
2114:
1935:Terra Sabaea
1875:Arabia Terra
1738:(1): 36–62.
1735:
1731:
1725:
1716:
1689:
1683:
1658:
1654:
1648:
1605:
1601:
1595:
1560:
1556:
1546:
1519:
1515:
1505:
1483:(E3): 5639.
1480:
1476:
1466:
1437:
1433:
1423:
1406:
1402:
1395:
1360:
1356:
1346:
1311:
1307:
1297:
1262:
1258:
1248:
1215:
1211:
1205:
1156:
1152:
1146:
1097:
1093:
1087:
1046:
1042:
1036:
1011:
1007:
1001:
966:
962:
952:
933:
929:
919:
884:
878:
865:
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831:
827:
821:
796:
792:
750:
746:
740:
705:
701:
691:
666:
662:
656:
635:
627:
602:
598:
592:
576:
567:
548:
542:
517:
513:
500:
491:
407:
388:
382:
341:
230:
221:eccentricity
206:
197:
185:
176:
168:
155:
144:
129:
120:
113:
103:STL 3D model
86:
54:
51:
36:
31:
25:
2545:Exploration
2467:5261 Eureka
2135:Groundwater
2100:Composition
1925:Tempe Terra
1915:Quadrangles
1842:Circulation
1772:Google Maps
1768:Google Mars
381:(See also:
378:are noted.
194:Dust storms
2202:Polar caps
2182:Mud cracks
2165:Meteorites
2150:Lava tubes
2085:Carbonates
2020:Labyrinthi
1895:Iani Chaos
1834:Atmosphere
1447:2212.02466
1440:: 115395.
636:Mars: Maps
484:References
360:−8 km
340:on NASA's
334:elevations
330:your mouse
182:Atmosphere
139:See also:
2727:Sub-Earth
2710:Mythology
2663:Mars race
2430:Asteroids
2326:Astronomy
2297:Hesperian
2292:Amazonian
2264:Volcanism
2239:Spherules
2160:Marsquake
2115:Dichotomy
2030:by height
2025:Mountains
1825:Geography
1708:232551466
1615:1210.3838
1587:2197-4284
1563:(1): 18.
1387:1944-8007
1338:1944-8007
1289:1944-8007
1181:0028-0836
1122:0028-0836
993:2156-2202
911:132406061
799:: 78–95.
732:2156-2202
372:longitude
356:0 km
213:solstices
209:precesses
163:Hesperian
161:to early
2813:Category
2763:Category
2627:Advocacy
2610:Missions
2553:Concepts
2382:Transits
2353:Monolith
2302:Noachian
2274:Yardangs
2170:on Earth
2130:Glaciers
1975:"Canals"
1967:features
1965:Physical
1640:19823214
1189:18580944
1130:18580945
1071:18580944
870:Archived
775:26520111
412:See also
368:latitude
328:. Hover
159:Noachian
2695:Fiction
2676:Related
2570:Landing
2565:Orbiter
2524:General
2493:2007 NS
2483:1999 UJ
2473:1998 VF
2462:Trojans
2449:2007 WD
2438:Impacts
2418:Mercury
2284:History
2244:Surface
2175:on Mars
2140:Gullies
2125:Geysers
2072:Geology
2062:Gravity
2057:Valleys
2010:Gullies
2000:Craters
1990:Catenae
1985:Canyons
1940:Tharsis
1885:Cydonia
1867:Regions
1857:Methane
1847:Climate
1740:Bibcode
1663:Bibcode
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