Alba Mons (formerly and still occasionally known as Alba Patera , a term that has since been restricted to the volcano's summit caldera; also initially known as the Arcadia ring ) is a volcano located in the northern Tharsis region of the planet Mars . It is the biggest volcano on Mars in terms of surface area, with volcanic flow fields that extend for at least 1,350 km (840 mi) from its summit. Although the volcano has a span comparable to that of the United States , it reaches an elevation of only 6.8 km (22,000 ft) at its highest point. This is about one-third the height of Olympus Mons , the tallest volcano on the planet. The flanks of Alba Mons have very gentle slopes. The average slope along the volcano's northern (and steepest) flank is 0.5°, which is over five times lower than the slopes on the other large Tharsis volcanoes . In broad profile, Alba Mons resembles a vast but barely raised welt on the planet's surface. It is a unique volcanic structure with no counterpart on Earth or elsewhere on Mars.
76-404: In addition to its great size and low relief , Alba Mons has a number of other distinguishing features. The central portion of the volcano is surrounded by an incomplete ring of faults ( graben ) and fractures, called Alba Fossae on the volcano's western flank and Tantalus Fossae on the eastern flank. The volcano also has very long, well preserved lava flows that form a radiating pattern from
152-491: A planet , moon , or asteroid . A "global DEM" refers to a discrete global grid . DEMs are used often in geographic information systems (GIS), and are the most common basis for digitally produced relief maps . A digital terrain model (DTM) represents specifically the ground surface while DEM and DSM may represent tree top canopy or building roofs. [REDACTED] The dictionary definition of terrain at Wiktionary Ceraunius Fossae The Ceraunius Fossae are
228-618: A branching pattern of shallow gullies and channels ( valley networks ) that likely formed by water runoff. Alba Mons has some of the oldest extensively exposed volcanic deposits in the Tharsis region. Geologic evidence indicates that significant volcanic activity ended much earlier at Alba Mons than at Olympus Mons and the Tharsis Montes volcanoes. Volcanic deposits from Alba Mons range in age from Hesperian to early Amazonian (approximately 3.6 to 3.2 billion years old). For years
304-519: A distance of over 1000 km. The southern half of the Alba Mons volcano is built over the northern extension of this ridge. The Ceraunius Fossae are tectonic features indicating stresses in the planet's lithosphere . The fractures form when the stresses exceed the yield strength of rock, resulting in deformation of surface materials. Typically, this deformation is manifested as slip on faults that are recognizable in images from orbit. Most of
380-402: A downfaulted block of crust (pictured right). Alba has perhaps the clearest display of simple graben on the entire planet. Alba's graben are up to 1,000 km (620 mi) long, and have a width on the order of 2 km (1.2 mi)–10 km (6.2 mi), with depths of 100 m (330 ft)–350 m (1,150 ft). Tension cracks (or joints ) are extensional features produced when
456-590: A long, narrow depression or trench. The International Astronomical Union (IAU) formally adopted the term Ceraunius Fossae in 1973. The name Ceraunius Fossae is plural and translates into "the Ceraunian trenches". Most of the Ceraunius Fossae are located in the northern Tharsis quadrangle . A portion extend northward into the southwestern part of the Arcadia quadrangle where the fossae diverge around
532-405: A peculiar concentric circular feature 10 km (6.2 mi) in diameter (pictured left). Calderas form by collapse following withdrawal and depletion of a magma chamber after an eruption. Caldera dimensions allow scientists to infer the geometry and depth of the magma chamber beneath the summit of the volcano. The shallowness of Alba's calderas compared to those seen on Olympus Mons and most of
608-685: A regional pattern of radiating graben and rifts is consistent with stresses caused by loading of the lithosphere by the enormous weight of the Tharsis bulge. The immense Valles Marineris is probably the best known example of a rift system that lies radial to Tharsis. Several generations of grabens with slightly different orientations are present in Ceraunius Fossae, indicating that stress fields have changed somewhat over time. In addition to producing normal faults and graben, extensional stresses can produce dilatant fractures or tension cracks that can open up subsurface voids. When surface material slides into
684-405: A relatively recent, Amazonian -aged glacial epoch. In summary, current geologic analysis of Alba Mons suggests that the volcano was built by lavas with rheological properties similar to basalts . If early explosive activity happened at Alba Mons, the evidence (in the form of extensive ash deposits) is largely buried by younger basaltic lavas. The immense system of fractures surrounding Alba Mons
760-460: A set of fractures in the northern Tharsis region of Mars . They lie directly south of the large volcano Alba Mons and consist of numerous parallel faults and tension cracks that deform the ancient highland crust. In places, younger lava flows cover the fractured terrain, dividing it into several large patches or islands. They are found in the Tharsis quadrangle . The faults are mainly narrow, north-south oriented graben . Graben (the name
836-433: A time of more focused effusive activity consisting of long tube- and channel-fed flows. Volcanic spreading occurred in a northward direction forming the two flanking lobes. (See Olympus Mons and Tharsis for a discussion of volcanic spreading on Mars.) Faulting and graben formation at Alba and Tantalus Fossae occurred penecontemporaneous with the lava flows. Any early explosive activity on the volcano may have occurred during
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#1732787473939912-433: A vast, nearly level apron of lava flows that extends an additional 1,000 km (620 mi) or so outward. The central body is the main topographic edifice of the volcano, marked by pronounced break in slope at the inner boundary of the apron. Extending east and west from the central edifice are two broad fan-shaped lobes (or shoulders), which give the volcano its elongation in the east-west direction. The central edifice has
988-413: A volume of about 2.5 million km. The volcano dominates the northern portion of the Tharsis bulge and is so large and geologically distinct that it can almost be treated as an entire volcanic province unto itself. Although Alba Mons reaches a maximum elevation of 6.8 km (22,000 ft) above Mars’ datum , the elevation difference between its summit and surrounding terrain (relief) is much greater on
1064-519: Is both singular and plural) are long, narrow troughs bound by two inward-facing normal faults that enclose a downfaulted block of crust. The graben in the Ceraunius Fossae are commonly several kilometers wide, between 100 and slightly over 1000 m deep, and very closely spaced, giving the terrain a rugged ridge and groove topography . Many of the graben are hundreds of kilometers long and have walls with complex scalloped segments. Some contain pit crater chains (catenae) at their bottoms, suggesting
1140-638: Is built on a broad, north-south topographic ridge that corresponds to the fractured, Noachian-aged terrain of Ceraunius Fossae (pictured left). Alba's size and low profile makes it a difficult structure to study visually, as much of the volcano's relief is indiscernible in orbital photographs. However, between 1997 and 2001, the Mars Orbital Laser Altimeter (MOLA) instrument of the Mars Global Surveyor spacecraft took over 670 million precise elevation measurements across
1216-469: Is characterized by sets of low, flat-topped ridges that form a radial pattern extending for hundreds of kilometers to the west, north, and northeast of the main edifice. The ridges are interpreted to be lava flows, although the flow margins are now degraded and difficult to delineate. Broad lava flows with flat-topped ridges are characteristic features of lava flood provinces on Earth (e.g., Columbia River basalt ) that were formed at high eruption rates. Thus,
1292-406: Is outlined everywhere by a steep wall that varies in height over a range of a few hundred meters. The walls of both calderas are scalloped, suggesting multiple episodes of subsidence and/or mass wasting . Two small shields or domes, several hundred meters high, occur within and adjacent to the large caldera. The shield within the large caldera is about 50 km (31 mi) across. It is capped by
1368-664: Is perhaps the most striking feature of the volcano. The fractures are tectonic features indicating stresses in the planet's lithosphere . They form when the stresses exceed the yield strength of rock, resulting in the deformation of surface materials. Typically, this deformation is manifested as slip on faults that are recognizable in images from orbit. Alba's tectonic features are almost entirely extensional, consisting of normal faults , graben and tension cracks. The most common extensional features on Alba Mons (and Mars in general) are simple graben . Graben are long, narrow troughs bound by two inward-facing normal faults that enclose
1444-466: Is the lay of the land. This is usually expressed in terms of the elevation , slope , and orientation of terrain features. Terrain affects surface water flow and distribution. Over a large area, it can affect weather and climate patterns. Bathymetry is the study of underwater relief, while hypsometry studies terrain relative to sea level . The understanding of terrain is critical for many reasons: Relief (or local relief ) refers specifically to
1520-414: Is unstable at these locations under present conditions and will tend to sublimate into the atmosphere. Theoretical calculations indicate that remnant ice can be preserved below depths of 1 m if it is blanketed by a high-albedo and low-thermal-inertia material, such as dust. The mineral composition of rocks making up Alba Mons is difficult to determine from orbital reflectance spectrometry because of
1596-556: Is within the range of the highest terrestrial volcanic flows, such as the 1984 Mauna Loa , North Queensland ( McBride Province ), and the Columbia River basalts. The highest range is several orders of magnitude higher than the effusive rates for any terrestrial volcano. Since the late 1980s, some researchers have suspected that Alba Mons eruptions included a significant amount of pyroclastics (and therefore explosive activity) during early phases of its development. The evidence
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#17327874739391672-780: The Mars Reconnaissance Orbiter (MRO) shows a line of rimless pit craters in Cyane Fossae on the Alba's western flank (pictured right). The pits likely formed by the collapse of surface materials into open fractures created as magma intruded the subsurface rock to form dikes . The northern slopes of Alba Mons contain numerous branching channel systems or valley networks that superficially resemble drainage features produced on Earth by rainfall. Alba's valley networks were identified in Mariner 9 and Viking images in
1748-460: The regolith just below the surface on Alba's northern flank may contain 7.6% WEH by mass. This concentration could indicate water present as remnant ice or in hydrated minerals. Alba Mons is one of several areas on the planet that may contain thick deposits of near-surface ice preserved from an earlier epoch (1 to 10 million years ago), when Mars’ axial tilt (obliquity) was higher and mountain glaciers existed at mid-latitudes and tropics. Water ice
1824-529: The 1970s, and their origin has long been a topic of Mars research. Valley networks are most common in the ancient Noachian-aged southern highlands of Mars, but also occur on the flanks of some of the large volcanoes. The valley networks on Alba Mons are Amazonian in age and thus significantly younger than the majority of those in the southern highlands. This fact presents a problem for researchers who propose that valley networks were carved by rainfall runoff during an early, warm and wet period of Martian history. If
1900-403: The Alba and Tantalus Fossae fracture ring, but the actual vents for the sheet flows are not visible and may have been buried by their own products. Flow thicknesses have been measured for a number of sheet flows based on MOLA data. The flows range from 20 m (66 ft) to 130 m (430 ft) thick and are generally thickest at their distal margins. The second major type of lava flows on
1976-473: The Arcadia Ring (in reference to the partial ring of fractures around the volcano). The IAU named the volcano Alba Patera in 1973. The volcano is often simply called Alba when the context is understood. Alba Mons is centered at 40°28′N 250°24′E / 40.47°N 250.4°E / 40.47; 250.4 in the Arcadia quadrangle (MC-3). Much of the volcano's western flank is located in
2052-559: The Hellas impact basin, a few researchers have conjectured that the volcano's formation may have been related to crustal weakening from the Hellas impact, which produced strong seismic waves that focused on the opposite side of the planet. Terrain Terrain (from Latin : terra 'earth'), alternatively relief or topographical relief , is the dimension and shape of a given surface of land . In physical geography , terrain
2128-417: The adjacent Diacria quadrangle (MC-2). Flows from the volcano can be found as far north as 61°N and as far south as 26°N (in the northern Tharsis quadrangle ). If one takes the outer margin of the flows as the volcano's base, then Alba Mons has north–south dimensions of about 2,000 km (1,200 mi) and a maximum width of 3,000 km (1,900 mi). It covers an area of at least 5.7 million km and has
2204-524: The apron area farther to the north. This suggests that the northern portions of Alba's surface may contain a higher abundance of duricrusts , sand, and rocks compared to the rest of the volcano. High thermal inertia can also indicate the presence of exposed water ice. Theoretical models of water-equivalent hydrogen (WEH) from epithermal neutrons detected by the Mars Odyssey Neutron Spectrometer (MONS) instrument suggest that
2280-435: The center of Tharsis and are likely a crustal response to the sagging weight of the Tharsis bulge. The faults ringing Alba's summit region may be due to a combination of loading from the Alba edifice and magma uplift or underplating from the underlying mantle. Some of the fractures are likely the surface expression of gigantic dike swarms radial to Tharsis. An image from High Resolution Imaging Science Experiment ( HiRISE ) on
2356-442: The central edifice of Alba Mons resembles a partially collapsed shield volcano with a smaller, summit dome sitting on top (pictured right). The summit dome has a distinct tilt to the east. The caldera complex consists of a large caldera about 170 km (110 mi) by 100 km (62 mi) across at the center of the summit dome. A smaller, kidney-shaped caldera (about 65 km (40 mi) by 45 km (28 mi)) lies in
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2432-408: The climate conditions changed billions of years ago into today's cold and dry Mars (where rainfall is impossible), how does one explain the younger valleys on Alba Mons? Did Alba's valley networks form differently from those in the highlands, and if so, how? Why do the valleys on Alba Mons occur mainly on the northern flanks of the volcano? These questions are still being debated. In Viking images,
2508-493: The constructional volcanic activity at Alba is believed to have occurred within a relatively brief time interval (about 400 million years) of Mars history, spanning mostly the late Hesperian to very early Amazonian epochs. Faulting and graben formation in the region occurred in two early stages: one preceding and the other contemporaneous with the volcano's formation. Two late stages of graben formation occurred after volcanic activity had largely ended. Based on Viking Orbiter images,
2584-442: The crust is wrenched apart with no significant slippage between the separated rock masses. In theory they should appear as deep fissures with sharp V-shaped profiles, but in practice they are often difficult to distinguish from graben because their interiors rapidly fill with talus from the surrounding walls to produce relatively flat, graben-like floors. Pit crater chains (catenae), common within many graben on Alba's flanks, may be
2660-558: The culmination of this middle phase of activity, which ended about 3400 million years ago. The youngest unit, also early Amazonian, covers the summit plateau, dome, and caldera complex. This period of activity is characterized by relatively short-length sheet flows and construction of the summit dome and the large caldera. This phase ended with an eastward tilting of the summit dome, which may have initiated additional graben formation in Alba Fossae. The last volcanic features to form were
2736-418: The earliest phase of volcanic activity at Alba Mons probably involved massive effusive eruptions of low viscosity lavas that formed the volcano's broad, flat apron. Lava flows of the apron unit straddle the early Hesperian-late Hesperian boundary, having erupted approximately 3700 to 3500 million years ago. The middle unit, which is early Amazonian in age, makes up the flanks of the main Alba edifice and records
2812-448: The early 1970s. Much of the geologic work on Alba Mons has focused on the morphology of its lava flows and the geometry of the faults cutting its flanks. Surface features of the volcano, such as gullies and valley networks, have also been extensively studied. These efforts have the overall goal of deciphering the geologic history of the volcano and the volcano-tectonic processes involved in its formation. Such understanding can shed light on
2888-478: The edifice were built largely from pyroclastic flow deposits ( ignimbrites ). More recent data from Mars Global Surveyor and the Mars Odyssey spacecraft have shown no specific evidence that explosive eruptions ever occurred at Alba Mons. An alternative explanation for the valley networks on the north side of the volcano is that they were produced through sapping or melting of ice-rich dust deposited during
2964-601: The edifice. In high resolution images, many of the flows on the volcano's upper flanks originally characterized as sheet flows have central channels with levee-like ridges. The morphology of lava flows can indicate properties of the lava when molten, such as its rheology and flow volume. Together, these properties can provide clues to the lava's composition and eruption rates. For example, lava tubes on Earth only form in lavas of basaltic composition. Silica -rich lavas such as andesite are too viscous for tubes to form. Early quantitative analysis of Alba's lava flows indicated that
3040-419: The eroded material is an ice-rich dust or friable volcanic ash is still uncertain. Alba's well-preserved lava flows and faults provide an excellent photogeologic record of the volcano's evolution. Using crater counting and basic principles of stratigraphy , such as superposition and cross-cutting relationships , geologists have been able to reconstruct much of Alba's geologic and tectonic history. Most of
3116-400: The flanks of Alba Mons are called tube- and channel-fed flows, or crested flows. They form long, sinuous ridges that radiate outward from the central region of the volcano. They are typically 5 km (3.1 mi)-10 km (6.2 mi) wide. An individual ridge may have a discontinuous channel or line of pits that run along its crest. Tube- and channel-fed flows are particularly prominent on
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3192-464: The flanks of Alba Mons to form the Alba and Tantalus Fossae systems. The area stretches from lat. 18.9° to 38°N and from long. 247° to 255°E. The entire feature has a north-south length of 1137 km. The Ceraunius Fossae lie on a broad topographic ridge up to 1.5 km high, called the Ceraunius rise. The ridge projects from the southern edge of Alba Mons and extends southward for
3268-422: The flanks of the volcano, forming an incomplete ring about 500 km (310 mi) in diameter. The set of faults on Alba's western flank is called Alba Fossae and the one on the eastern flank Tantalus Fossae . North of the volcano, the faults splay outward in a northeasterly directions for distances of many hundreds of kilometers. The pattern of faults curving around Alba's flanks has been likened in appearance to
3344-419: The full range of their interactions is still a topic of debate. Land surface parameters are quantitative measures of various morphometric properties of a surface. The most common examples are used to derive slope or aspect of a terrain or curvatures at each location. These measures can also be used to derive hydrological parameters that reflect flow/erosion processes. Climatic parameters are based on
3420-441: The grain of a piece of wood running past a knot. The entire Ceraunius-Alba-Tantalus fault system is at least 3,000 km (1,900 mi) long and 900 km (560 mi)–1,000 km (620 mi) wide Several causes for the faults have been suggested, including regional stresses created by the Tharsis bulge, volcanic dikes, and crustal loading by Alba Mons itself. The faults of Ceraunius and Tantalus Fossae are roughly radial to
3496-616: The lavas had low yield strength and viscosity and were erupted at very high rates. Alba's unusually low profile suggested to some that extremely fluid lavas were involved in the volcano's construction, perhaps komatiites , which are primitive ultramafic lavas that form at very high temperatures. However, more recent work on the tube- and channel-fed flows indicates lava viscosities within the range of typical basalts (between 100 and 1 million Pa s). Calculated flow rates are also lower than originally thought, ranging from 10 to 1.3 million m per second. The lower range of eruption rates for Alba Mons
3572-506: The modelling of solar radiation or air flow. Land surface objects, or landforms , are definite physical objects (lines, points, areas) that differ from the surrounding objects. The most typical examples airlines of watersheds , stream patterns, ridges , break-lines , pools or borders of specific landforms. A digital elevation model (DEM) or digital surface model (DSM) is a 3D computer graphics representation of elevation data to represent terrain or overlaying objects, commonly of
3648-556: The nature and evolution of the Martian interior and the planet's climate history. Alba Mons is notable for the remarkable length, diversity, and crisp appearance of its lava flows. Many of the flows radiate from the summit, but others appear to originate from vents and fissures on the lower flanks of the volcano. Individual flows may exceed 500 km (310 mi) in length. Lava flows near the summit calderas appear to be significantly shorter and narrower than those on more distal parts of
3724-484: The near future. The thick mantle of dust obscures the underlying bedrock, probably making in situ rock samples hard to come by and thus reducing the site's scientific value. The dust layer would also likely cause severe maneuvering problems for rovers. Ironically, the summit region was originally considered a prime backup landing site for the Viking 2 lander because the area appeared so smooth in Mariner 9 images taken in
3800-581: The north side of the volcano (about 7.1 km (23,000 ft)) compared to the south side (about 2.6 km (8,500 ft)). The reason for this asymmetry is that Alba straddles the dichotomy boundary between the cratered uplands in the south and the lowlands to the north. The plains underlying the volcano slope northward toward the Vastitas Borealis , which has an average surface elevation of 4.5 km (15,000 ft) below datum (-4.500 km (14,760 ft)). The southern part of Alba Mons
3876-499: The other Tharsis volcanoes implies that Alba's magma reservoir was wider and shallower than those of its neighbors. Most of the central edifice of Alba Mons is mantled with a layer of dust approximately 2 m (6.6 ft) thick. The dust layer is visible in high resolution images of the summit (pictured right). In places, the dust has been carved into streamlined shapes by the wind and is cut by small landslides . However, some isolated patches of dust appear smooth and undisturbed by
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#17327874739393952-401: The planet. Using MOLA data, planetary scientists are able to study subtle details of the volcano's shape and topography that were invisible in images from earlier spacecraft such as Viking . The volcano consists of two, roughly concentric components: 1) an oval-shaped central body with approximate dimensions of 1,500 km (930 mi) by 1,000 km (620 mi) across surrounded by 2)
4028-428: The predominance of surface dust throughout the region. However, global-scale surface composition can be inferred from the Mars Odyssey gamma-ray spectrometer (GRS). This instrument has allowed scientists to determine the distribution of hydrogen (H), silicon (Si), iron (Fe), chlorine (Cl), thorium (Th) and potassium (K) in the shallow subsurface. Multivariate analysis of GRS data indicates that Alba Mons and
4104-490: The presence of deep-seated tension cracks into which surface material has drained. The term Ceraunius is from an albedo feature at lat. 19.78°N, long. 267°E. It was named by Greek Astronomer E. M. Antoniadi in 1930 for the Ceraunian Mountains on the coast of Epirus , Greece (now southwestern Albania ). Fossa (pl. fossae ) is Latin for ditch and is a descriptor term used in planetary geology for
4180-410: The quantitative measurement of vertical elevation change in a landscape . It is the difference between maximum and minimum elevations within a given area, usually of limited extent. A relief can be described qualitatively, such as a " low relief " or " high relief " plain or upland . The relief of a landscape can change with the size of the area over which it is measured, making the definition of
4256-576: The resemblance of Alba's valley networks to terrestrial pluvial (rainfall) valleys is quite striking. The valley networks show a fine-textured, parallel to dendritic pattern with well-integrated tributary valleys and drainage densities comparable to those on Earth's Hawaiian volcanoes. However, stereoscopic images from the High Resolution Stereo Camera (HRSC) on the European Mars Express orbiter show that
4332-417: The rest of the Tharsis region belongs to a chemically distinct province characterized by relatively low Si (19 wt%), Th (0.58 pppm), and K (0.29 wt%) content, but with Cl abundance (0.56 wt%) higher than Mars' surface average. Low silicon content is indicative of mafic and ultramafic igneous rocks, such as basalt and dunite . Alba Mons is an unlikely target for unmanned landers in
4408-476: The scale over which it is measured very important. Because it is related to the slope of surfaces within the area of interest and to the gradient of any streams present, the relief of a landscape is a useful metric in the study of the Earth's surface. Relief energy, which may be defined inter alia as "the maximum height range in a regular grid", is essentially an indication of the ruggedness or relative height of
4484-471: The small shield and caldera at the summit. Much later, between about 1,000 and 500 million years ago, a final stage of faulting occurred that may have been related to dike emplacement and the formation of pit crater chains. The classification of the Alba Mons volcano is uncertain. Some workers describe it as a shield volcano , others as a lowland patera (in contrast to highland paterae , which are low-lying ancient volcanoes with furrowed ash deposits located in
4560-595: The southern Martian highlands), and still others consider it a one-of-a-kind volcanic structure unique to Mars. Some researchers have compared Alba Mons to coronae structures on the planet Venus . Alba Mons shares some characteristics with the Syrtis Major volcanic structure. (See Volcanism on Mars .) Both volcanoes are Hesperian in age, cover large areas, have very low relief, and large shallow calderas. Also like Alba, Syrtis Major displays ridged tube- and channel-fed lava flows. Because Alba Mons lies antipodal to
4636-430: The southern half of the larger one. Both calderas are relatively shallow, reaching a maximum depth of only 1.2 km (3,900 ft). The larger caldera is bounded at the westernmost end by a steep, semicircular wall 500 m (1,600 ft) tall. This wall disappears at the northern and southern sides of the caldera, where it is buried by volcanic flows originating from the younger, smaller caldera. The smaller caldera
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#17327874739394712-431: The steepest slopes on the volcano, although they are still only 1°. The crest and upper flanks of the edifice are cut by a partial ring of graben that are part of the Alba and Tantalus Fossae fracture system. Inside the ring of graben is an annulus of very low and in places reversed slopes that forms a plateau on top of which lies a central dome 350 km (220 mi) across capped by a nested caldera complex. Thus,
4788-502: The surface manifestation of deep tension cracks into which surface material has drained. The graben and fractures around Alba Mons (hereafter simply called faults unless otherwise indicated) occur in swarms that go by different names depending on their location with respect to Alba's center. South of the volcano is a broad region of intensely fractured terrain called Ceraunius Fossae , which consists of roughly parallel arrays of narrow, north-south oriented faults. These faults diverge around
4864-416: The tectonic features in the western hemisphere of Mars are explained by crustal deformation from the Tharsis bulge (a huge volcanic mass up to 7 km high that covers nearly a quarter of the planet’s surface). Among the processes proposed to explain the tectonic features associated with Tharsis are domal uplifting, magmatic intrusion , and volcanic loading (deformation due to the large, sagging weight of
4940-544: The terrain. Geomorphology is in large part the study of the formation of terrain or topography. Terrain is formed by concurrent processes operating on the underlying geological structures over geological time : Tectonic processes such as orogenies and uplifts cause land to be elevated, whereas erosional and weathering processes wear the land away by smoothing and reducing topographic features. The relationship of erosion and tectonics rarely (if ever) reaches equilibrium. These processes are also codependent, however
5016-463: The valleys are relatively shallow (30 m (98 ft) or less) and more closely resemble rills or gullies from intermittent runoff erosion than valleys formed from sustained erosion. It seems likely that the valleys on Alba Mons formed as a result of transient erosional processes, possibly related to snow or ice deposits melting during volcanic activity, or to short-lived periods of global climate change. (See Surface characteristics, above.) Whether
5092-451: The void, a pit crater may form. Pit craters are distinguishable from impact craters in lacking raised rims and surrounding ejecta blankets . On Mars, individual pit craters can coalesce to form crater chains (catenae) or troughs with scalloped edges. Evidence also exists that some of the graben and crater chains in the Ceraunius Fossae may have been formed by the intrusion of magma , which forms large underground dikes . The migration of
5168-483: The volcanic mass). The Ceraunius Fossae fractures are extensional features produced when the crust is stretched apart. The fractures are oriented north-south, radial to an early center of volcano-tectonic activity in Syria Planum , a region in southern Tharsis. A large number of extensional structures, including graben and rifts , radiate outward from the center of Tharsis. Mechanical studies indicate that
5244-498: The volcanic materials related to the formation and evolution of the volcano have been grouped into the Alba Patera Formation , which consists of lower, middle, and upper members . Members low in the stratigraphic sequence are older than those lying above, in accordance with Steno's law of superposition . The oldest unit (lower member) corresponds to the broad lava apron surrounding the Alba Mons edifice. This unit
5320-400: The volcano's central region. The enormous lengths of some individual flows (>300 km (190 mi)) implies that the lavas were very fluid (low viscosity ) and of high volume. Many of the flows have distinctive morphologies, consisting of long, sinuous ridges with discontinuous central lava channels. The low areas between the ridges (particularly along the volcano's northern flank) show
5396-508: The volcano's formal name was Alba Patera. Patera (pl. paterae ) is Latin for a shallow drinking bowl or saucer. The term was applied to certain ill-defined, scalloped-edged craters that appeared in early spacecraft images to be volcanic (or non- impact ) in origin. In September 2007, the International Astronomical Union (IAU) renamed the volcano Alba Mons (Alba Mountain), reserving the term Alba Patera for
5472-467: The volcano's two central depressions ( calderas ). Nevertheless, the entire volcano is still commonly called Alba Patera in the planetary science literature. The term Alba is from the Latin word for white and refers to the clouds frequently seen over the region from Earth-based telescopes. The volcano was discovered by the Mariner 9 spacecraft in 1972 and was initially known as the Alba volcanic feature or
5548-462: The volcano. The two most common types of volcanic flows on Alba Mons are sheet flows and tube-and-channel fed flows. Sheet flows (also called tabular flows) form multiple, overlapping lobes with steep margins. The flows typically lack central channels. They are flat-topped and generally about 5 km (3.1 mi) wide on the upper flanks of the volcano but become much wider and lobate toward their downstream (distal) ends. Most appear to originate near
5624-676: The western flank of the volcano where individual ridges can be traced for several hundred kilometers. The origin of the ridges is uncertain. They may form by successive buildup of solidified lava at the mouth of a channel or tube, with each pulse of flowing lava adding to the length of the ridge. In addition to the two main types of flows, numerous undifferentiated flows are present around Alba Mons that are either too degraded to characterize or have hybrid characteristics. Flat-topped ridges with indistinct margins and rugged surfaces, interpreted as lava flows, are common along Alba's lower flanks and become less sharp in appearance with increasing distance from
5700-453: The wind. Heavy dust cover is also indicated by the high albedo (reflectivity) and low thermal inertia of the region. Martian dust is visually bright (albedo > 0.27) and has a low thermal inertia because of its small grain size (<40 μm (0.0016 in)). (See the Martian surface .) However, the thermal inertia is high and albedo lower on the northern flanks of the volcano and in
5776-401: Was based on the presence of numerous valley networks on the volcano's northern flanks that appeared to be carved by running water (see below). This evidence combined with thermal inertia data, which indicated a surface dominated by fine-grained materials, suggested an easily erodible material, such as volcanic ash, was present. The volcano's extremely low profile is also more easily explained if
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