Arabia Terra is a large upland region in the north of Mars in that lies mostly in the Arabia quadrangle, but a small part is in the Mare Acidalium quadrangle. It is densely cratered and heavily eroded. This battered topography indicates great age, and Arabia Terra is presumed to be one of the oldest terrains on the planet. It covers as much as 4,500 km (2,800 mi) at its longest extent, centered roughly at Coordinates:  with its eastern and southern regions rising 4 km (13,000 ft) above the north-west. Alongside its many craters, canyons wind through the Arabia Terra, many emptying into the large northern lowlands of the planet, which borders Arabia Terra to the north.
Arabia contains many interesting features. There are some good examples of pedestal craters in the area. A pedestal crater has its ejecta above the surrounding terrain, often forming a steep cliff. The ejecta forms a resistant layer that protects the underlying material from erosion. Mounds and buttes on the floor of some craters display many layers. The layers may have formed by volcanic processes, by wind, or by underwater deposition. Dark slope streaks have been observed in Tikhonravov Basin, a large eroded crater. The streaks appear on steep slopes and change over time. At first they are dark, then turn a lighter color, probably by the deposition of fine, light colored dust from the atmosphere.These streaks are thought to form by dust moving downslope in a way similar to snow avalanches on Earth.
Research on the region was undertaken in 1997 and the individuality of the province better defined. An equatorial belt was noted with a crater age distinctly younger than the northern part of the province and of Noachis Terra to the south. This was interpreted as an "incipient back-arc system" provoked by the subduction of Mars lowlands under Arabia Terra during Noachian times. Regional fracture patterns were also explained in this manner, and the rotational instability of the planet as a cause was not supported. It contains extension tectonic features
A 2013 study proposed that a number of craters within Arabia Terra, including Eden Patera, Euphrates Patera, Siloe Patera, and possibly Semeykin crater, Ismenia Patera, Oxus Patera and Oxus Cavus, represent calderas formed by massive explosive volcanic eruptions of Late Noachian to Early Hesperian age. Termed "plains-style caldera complexes", these very low relief volcanic features appear to be older than the large Hesperian-age shield volcanoes of Tharsis or Elysium. Eden Patera, for example, is an irregular, 55 by 85 km depression up to 1.8 km deep, surrounded by ridged basaltic plains. It contains three linked interior depressions, demarcated by arcuate scarps, that have terraces suggestive of lava lake drainage and faults suggestive of collapse. The features indicative of impact origin that would be expected in an impact crater of comparable diameter and depth are absent. The authors regard crustal thinning due to regional extension to be a more likely explanation for the origin of the volcanic activity than putative subduction. Rapid ascent of magma through the thin crust and a consequent relative absence of degassing may explain the more explosive eruption style associated with these paterae relative to that of the shield volcanoes. The eruptions would have contributed to the layered deposits of Arabia Terra, which are among the fine-grained deposits widespread in the equatorial regions of Mars. Total eruptive volumes of at least 4,600–7,200 km3 per caldera complex (over its history) were inferred.
Recent meteoroid impact
A meteorite impacted in Arabia Terra some time between 30 June 2002 and 5 October 2003. A single small crater of about 22.6 meters (about 74 feet) in diameter is surrounded by light and dark-toned ejecta - indicating that this impact excavated to a depth where light colored strata exists. The crater occurs near 20.6 degrees north latitude, 356.8 degrees west longitude, in Arabia Terra. Images of the area show how the impact site appeared to the Mars Odyssey Thermal Emission Imaging System infrared instrument before and after the impact. 
In popular culture
Many places on Mars show rocks arranged in layers. Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers. Layers may be formed by groundwater rising up depositing minerals and cementing sediments. The hardned layers are consequently more protected from erosion. This process may occur instead of layers forming under lakes.
A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars.
Tikonravev Crater floor, as seen by Mars Global Surveyor. Click on image to see dark slope streaks and layers.
Henry Crater mound, as seen by HiRISE. The scale bar is 500 m (1,600 ft) long
Crater in the middle of Cassini, as seen by HiRISE. Layers may have been deposited under water since it is believed that Cassini once held a giant lake.
Buttes, as seen by HiRISE under HiWish program. Buttes have layered rocks with a hard resistant cap rock on the top which protects the underlying rocks from erosion.
Many places on Mars show channels of different sizes. Many of these channels probably carried water, at least for a time. The climate of Mars may have been such in the past that water ran on its surface. It has been known for some time that Mars undergoes many large changes in its tilt or obliquity because its two small moons lack the gravity to stabilize it, as our moon stabilizes Earth; at times the tilt has even been greater than 80 degrees 
Channel in Arabia, as seen by HiRISE under HiWish program.
Close-up of channel within larger channel, as seen by HiRISE under HiWish program The existence of the smaller channel suggests water went through the region at least two times in the past. The black box represents the size of a football field. Some parts of the surface would be difficult to walk on with the many small hills and depressions.
An oblique view of Arabia Terra produced by Mars Global Surveyor
Wide view of mesa with CTX showing Cliff face and location of Lobate Debris Apron (LDA) Location is Ismenius Lacus quadrangle.
Enlargement of previous CTX image of mesa This image shows the cliff face and detail in the LDA. Image taken with HiRISE under HiWish program. Location is Ismenius Lacus quadrangle.
- Geography of Mars
- List of quadrangles on Mars
- Climate of Mars
- Geology of Mars
- Impact crater
- List of craters on Mars
|Wikimedia Commons has media related to Arabia Terra.|
- Blue, Jennifer. "Arabia Terra". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
- Anguita, F. et al. (1997). "Arabia Terra, Mars: Tectonic and Palaeoclimatic Evolution of a Remarkable Sector of Martian Lithosphere". Earth, Moon, and Planets 77 (1): 55. Bibcode:1997EM&P...77...55A. doi:10.1023/A:1006143106970.
- Brugman, K., B. Hynek, S. Robbins. 2015. CRATER-BASED TESTS UNLOCK THE MYSTERY OF THE ORIGIN AND EVOLUTION OF ARABIA TERRA, MARS. Lunar and Planetary Science Conference 2359.pdf
- "Eden Patera". USGS planetary nomenclature page. USGS. Retrieved 2013-10-17.
- "Euphrates Patera". USGS planetary nomenclature page. USGS. Retrieved 2013-10-17.
- "Siloe Patera". USGS planetary nomenclature page. USGS. Retrieved 2013-10-17.
- "Semeykin". USGS planetary nomenclature page. USGS. Retrieved 2013-10-17.
- "Ismenia Patera". USGS planetary nomenclature page. USGS. Retrieved 2013-10-17.
- "Oxus Patera". USGS planetary nomenclature page. USGS. Retrieved 2013-10-17.
- "Oxus Cavus". USGS planetary nomenclature page. USGS. Retrieved 2013-10-17.
- Witze, A. (2013). "Ancient supervolcanoes revealed on Mars". Nature. doi:10.1038/nature.2013.13857.
- Michalski, J. R.; Bleacher, J. E. (2013). "Supervolcanoes within an ancient volcanic province in Arabia Terra, Mars". Nature 502 (7469): 47–52. doi:10.1038/nature12482.
- Weir, Andy (2014). The Martian. New York: Crown Publishers. ISBN 978-0-8041-3902-1.
- "HiRISE | High Resolution Imaging Science Experiment". Hirise.lpl.arizona.edu?psp_008437_1750. Retrieved 2012-08-04.
- Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.
- name= Touma J. and J. Wisdom. 1993. The Chaotic Obliquity of Mars. Science 259, 1294-1297.
- Laskar, J., A. Correia, M. Gastineau, F. Joutel, B. Levrard, and P. Robutel. 2004. Long term evolution and chaotic diffusion of the insolation quantities of Mars. Icarus 170, 343-364.