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Phaethontis quadrangle
	; Map of Phaethontis quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are red and the lowest are blue.;
Coordinates	; 47°30′S 150°00′W / 47.5°S 150°W / -47.5; -150Coordinates: 47°30′S 150°00′W / 47.5°S 150°W / -47.5; -150;

Image of the Phaethontis Quadrangle (MC-24). The region is dominated by heavily cratered highlands and low-lying areas forming relatively smooth plains.

The Phaethontis quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Phaethontis quadrangle is also referred to as MC-24 (Mars Chart-24).^[1]

The name comes from Phaethon, the son of Helios.^[2]

The Phaethontis quadrangle lies between 30° and 65 ° south latitude and 120° and 180 ° west longitude on Mars. This latitude range is where numerous gullies have been discovered. An old feature in this area, called Terra Sirenum lies in this quadrangle; Mars Reconnaissance Orbiter discovered iron/magnesium smectites there.^[3] Part of this quadrangle contains what is called the Electris deposits, a deposit that is 100–200 meters thick. It is light-toned and appears to be weak because of few boulders.^[4] Among a group of large craters is Mariner Crater, first observed by the Mariner IV spacecraft in the summer of 1965. It was named after that spacecraft.^[5] A low area in Terra Sirenum is believed to have once held a lake that eventually drained through Ma'adim Vallis.^[6]^[7]^[8] Russia's Mars 3 probe landed in the Phaethontis quadrangle at 44.9° S and 160.1° W in December 1971. It landed at a speed of 75 km per hour, but survived to radio back 20 seconds of signal, then it went dead. Its message just appeared as a blank screen.^[9]

Martian gullies

The Phaethontis quadrangle is the location of many gullies that may be due to recent flowing water. Some are found in the Gorgonum Chaos^[10]^[11] and in many craters near the large craters Copernicus and Newton (Martian crater).^[12]^[13] Gullies occur on steep slopes, especially on the walls of craters. Gullies are believed to be relatively young because they have few, if any craters. Moreover, they lie on top of sand dunes which themselves are considered to be quite young. Usually, each gully has an alcove, channel, and apron. Some studies have found that gullies occur on slopes that face all directions,^[14] others have found that the greater number of gullies are found on poleward facing slopes, especially from 30-44 S.^[15]

Although many ideas have been put forward to explain them,^[16] the most popular involve liquid water coming from an aquifer, from melting at the base of old glaciers, or from the melting of ice in the ground when the climate was warmer.^[17]^[18] Because of the good possibility that liquid water was involved with their formation and that they could be very young, scientists are excited. Maybe the gullies are where we should go to find life.

There is evidence for all three theories. Most of the gully alcove heads occur at the same level, just as one would expect of an aquifer. Various measurements and calculations show that liquid water could exist in aquifers at the usual depths where gullies begin.^[17] One variation of this model is that rising hot magma could have melted ice in the ground and caused water to flow in aquifers. Aquifers are layer that allow water to flow. They may consist of porous sandstone. The aquifer layer would be perched on top of another layer that prevents water from going down (in geological terms it would be called impermeable). Because water in an aquifer is prevented from going down, the only direction the trapped water can flow is horizontally. Eventually, water could flow out onto the surface when the aquifer reaches a break—like a crater wall. The resulting flow of water could erode the wall to create gullies.^[19] Aquifers are quite common on Earth. A good example is "Weeping Rock" in Zion National Park Utah.^[20]

As for the next theory, much of the surface of Mars is covered by a thick smooth mantle that is thought to be a mixture of ice and dust.^[21]^[22]^[23] This ice-rich mantle, a few yards thick, smoothes the land, but in places it has a bumpy texture, resembling the surface of a basketball. The mantle may be like a glacier and under certain conditions the ice that is mixed in the mantle could melt and flow down the slopes and make gullies.^[24]^[25] Because there are few craters on this mantle, the mantle is relatively young. An excellent view of this mantle is shown below in the picture of the Ptolemaeus Crater Rim, as seen by HiRISE.^[26]
The ice-rich mantle may be the result of climate changes.^[27] Changes in Mars's orbit and tilt cause significant changes in the distribution of water ice from polar regions down to latitudes equivalent to Texas. During certain climate periods water vapor leaves polar ice and enters the atmosphere. The water comes back to ground at lower latitudes as deposits of frost or snow mixed generously with dust. The atmosphere of Mars contains a great deal of fine dust particles. Water vapor will condense on the particles, then fall down to the ground due to the additional weight of the water coating. When Mars is at its greatest tilt or obliquity, up to 2 cm of ice could be removed from the summer ice cap and deposited at midlatitudes. This movement of water could last for several thousand years and create a snow layer of up to around 10 meters thick.^[28]^[29] When ice at the top of the mantling layer goes back into the atmosphere, it leaves behind dust, which insulating the remaining ice.^[30] Measurements of altitudes and slopes of gullies support the idea that snowpacks or glaciers are associated with gullies. Steeper slopes have more shade which would preserve snow.^[15]
Higher elevations have far fewer gullies because ice would tend to sublimate more in the thin air of the higher altitude.^[31]

The third theory might be possible since climate changes may be enough to simply allow ice in the ground to melt and thus form the gullies. During a warmer climate, the first few meters of ground could thaw and produce a "debris flow" similar to those on the dry and cold Greenland east coast.^[32] Since the gullies occur on steep slopes only a small decrease of the shear strength of the soil particles is needed to begin the flow. Small amounts of liquid water from melted ground ice could be enough.^[33]^[34] Calculations show that a third of a mm of runoff can be produced each day for 50 days of each Martian year, even under current conditions.^[35]

Electris Deposit, as seen by HiRISE Electris deposit is light-toned and smooth in the image in contrast to rough materials below. Location is Phaethontis quadrangle.

Layers in light-toned Electris Deposit, as seen by HiRISE on the Mars Reconnaissance Orbiter. Gullies are visible on the left.

Gorgonum Chaos as seen by Mars Reconnaissance Orbiter HiRISE. Image about 4 km wide.

Group of gullies on north wall of crater that lies west of the crater Newton (41.3047 degrees south latitude, 192.89 east longitide). Image taken with Mars Global Surveyor under the MOC Public Targeting Program.

Crater wall inside Mariner Crater showing a large group of gullies, as seen by HiRISE.

Ptolemaeus Crater Rim, as seen by HiRISE. Click on image to see excellent view of mantle deposit.

Gullies. Notice how channels curve around obstacles, as seen by HiRISE.

Gullies with branches, as seen by HiRISE.

Group of deep gullies, as seen by HiRISE.

CTX image of the next image showing a wide view of the area. Since the hill is isolated it would be difficult for an aquifer to develop. Rectangle shows the approximate location of the next image.

Gully on mound as seen by Mars Global Surveyor, under the MOC Public Targeting Program. Images of gullies on isolated peaks, like this one, are difficult to explain with the theory of water coming from aquifers because aquifers need large collecting areas.

Another view of the previous gully on a mound. This one is with HiRISE, under the HiWish program. This view shows most of the apron and two old glaciers associated with it. All that is left of the glaciers are terminal moraines.

MOLA context image for the series of three images to follow of gullies in a trough and nearby crater.

Gullies in a trough and nearby crater, as seen by HiRISE under the HiWish program. Scale bar is 500 meters long.

Close-up of gullies in crater, as seen by HiRISE under the HiWish program.

Close-up of gullies in trough, as seen by HiRISE under the HiWish program. These are some of the smaller gullies visible on Mars.

Gullies near Newton Crater, as seen by HiRISE, under the HiWish program. Place where there was an old glacier is labeled.

HiRISE image, taken under HiWish program, of gullies in a crater in Terra Sirenum.

Gullies with remains of a former glacier in crater in Terra Sirenum, as seen by HiRISE under HiWish program.

Gullies near Newton Crater, as seen by HiRISE under the HiWish Program.

Gullies in a crater in Terra Sirenum, as seen by HiRISE under the HiWish Program.

Close-up of gully showing multiple channels and patterned ground, as seen by HiRISE under the HiWish program

Gullies in two levels of a crater wall, as seen by HiRISE under HiWish program. Gullies at two levels suggests they were not made with an aquifer, as was first suggested. Location is Phaethontis quadrangle.

Image of gullies with main parts labeled. The main parts of a Martian gully are alcove, channel, and apron. Since there are no craters on this gully, it is thought to be rather young. Picture was taken by HiRISE under HiWish program. Location is Phaethontis quadrangle.

Close-up of gully aprons showing they are free of craters; hence very young. Location is Phaethontis quadrangle. Picture was taken by HiRISE under HiWish program.

Gullies in crater, as seen by HiRISE under HiWish program. Location is Phaethontis quadrangle.

Close up of gullies in crater showing channels within larger valleys and curves in channels. These characteristics suggest they were made by flowing water. Note: this is an enlargement of the previous image by HiRISE under HiWish program. Location is Phaethontis quadrangle.

Close up of gully network showing branched channels and curves; these characteristics suggest creation by a fluid. Note: this is an enlargement of a previous wide view of gullies in a crater, as seen by HiRISE under HiWish program. Location is Phaethontis quadrangle.

Associated features of gullies

Sometimes other features appear near gullies. At the base of some gullies there may be depressions or curved ridges. These have been called "spatulate depressions." These depressions form after glacial ice disappears. Steep walls often develop glaciers during certain climates. When the climate changes, the ice in the glaciers sublimates in the thin Martian atmosphere. Sublimation is when a substance goes directly from a solid state to a gas state. Dry ice on Earth does this. So when the ice at the base of a steep wall sublimates, a depression results. Also, more ice from higher up will tend to flow downward. This flow will stretch the surface rocky debris thereby forming transverse crevasses. Such formations have been termed "washboard terrain" because they resemble the old fashioned washboards.^[36] The parts of gullies and some associated features of gullies are shown below in a HiRISE images.

Wide view of crater showing gullies and other features, as seen by HiRISE

Close view of crater labeled with "spatulate depression" and other features, as seen by HiRISE Note: this is an enlargement of the previous image.^[36]

Close view of crater labeled with "washboard terrain" and other features, as seen by HiRISE Note: this is an enlargement of a previous image. The washboard terrain was formed before the gully apron since the gully apron cuts across the washboard terrain.^[36]

Tongue-shaped glaciers

Tongue-shaped glacier, as seen by HiRISE under the HiWish program. Location is Phaethontis quadrangle.

Wide view of several tongue-shaped glaciers on wall of crater, as seen by HiRISE under the HiWish program. The glaciers are of different sizes and lie at different levels. Some of these are greatly enlarged in pictures which follow.

Close-up of the snouts of two glaciers from the previous image, as seen by HiRISE under the HiWish program. These are towards the bottom left of the previous image.

Close-up of small glaciers from a previous image, as seen by HiRISE under the HiWish program. Some of these glaciers seem to be just starting to form.

Close-up of the edge of one of the glaciers on the bottom of the wide view from a previous image Picture was taken by HiRISE under the HiWish program.

Possible pingos

The radial and concentric cracks visible here are common when forces penetrate a brittle layer, such as a rock thrown through a glass window. These particular fractures were probably created by something emerging from below the brittle Martian surface. Ice may have accumulated under the surface in a lens shape; thus making these cracked mounds. Ice being less dense than rock, pushed upwards on the surface and generated these spider web-like patterns. A similar process creates similar sized mounds in arctic tundra on Earth. Such features are called “pingos,”, an Inuit word.^[37] Pingos would contain pure water ice; thus they could be sources of water for future colonists of Mars.

Possible pingo, as seen by HiRISE under HiWish program

Possible pingos with scale, as seen by HiRISE under HiWish program

Close view of possible pingo with scale, as seen by HiRISE under HiWish program

Example of a pingo on Earth. On Earth the ice that caused the pingo would melt and fill the fractures with water; on Mars the ice would turn into a gas in the thin Martian atmosphere.

Concentric crater fill

Concentric crater fill, like lobate debris aprons and lineated valley fill, is believed to be ice-rich.^[38] Based on accurate topography measures of height at different points in these craters and calculations of how deep the craters should be based on their diameters, it is thought that the craters are 80% filled with mostly ice.^[39]^[40]^[41]^[42] That is, they hold hundreds of meters of material that probably consists of ice with a few tens of meters of surface debris.^[43]^[44] The ice accumulated in the crater from snowfall in previous climates.^[45]^[46]^[47] Recent modeling suggests that concentric crater fill develops over many cycles in which snow is deposited, then moves into the crater. Once inside the crater shade and dust preserve the snow. The snow changes to ice. The many concentric lines are created by the many cycles of snow accumulation. Generally snow accumulates whenever the axial tilt reaches 35 degrees.^[48]

Crater showing concentric crater fill, as seen by CTX (on Mars Reconnaissance Orbiter). Location is Phaethontis quadrangle.

Close-up view of concentric crater fill, as seen by HiRISE under HiWish program Note: this is an enlargement of previous image of a concentric crater. Location is Phaethontis quadrangle.

Wide view of concentric crater fill, as seen by CTX

Concentric crater fill, as seen by HiRISE under HiWish program

Close, color view of concentric crater fill, as seen by HiRISE under HiWish program

Magnetic stripes and plate tectonics

The Mars Global Surveyor (MGS) discovered magnetic stripes in the crust of Mars, especially in the Phaethontis and Eridania quadrangles (Terra Cimmeria and Terra Sirenum).^[49]^[50] The magnetometer on MGS discovered 100 km wide stripes of magnetized crust running roughly parallel for up to 2000 km. These stripes alternate in polarity with the north magnetic pole of one pointing up from the surface and the north magnetic pole of the next pointing down.^[51] When similar stripes were discovered on Earth in the 1960s, they were taken as evidence of plate tectonics. Researchers believe these magnetic stripes on Mars are evidence for a short, early period of plate tectonic activity. When the rocks became solid they retained the magnetism that existed at the time. A magnetic field of a planet is believed to be caused by fluid motions under the surface.^[52]^[53]^[54] However, there are some differences, between the magnetic stripes on Earth and those on Mars. The Martian stripes are wider, much more strongly magnetized, and do not appear to spread out from a middle crustal spreading zone.
Because the area containing the magnetic stripes is about 4 billion years old, it is believed that the global magnetic field probably lasted for only the first few hundred million years of Mars' life, when the temperature of the molten iron in the planet's core might have been high enough to mix it into a magnetic dynamo. There are no magnetic fields near large impact basins like Hellas. The shock of the impact may have erased the remnant magnetization in the rock. So, magnetism produced by early fluid motion in the core would not have existed after the impacts.^[55]

When molten rock containing magnetic material, such as hematite (Fe₂O₃), cools and solidifies in the presence of a magnetic field, it becomes magnetized and takes on the polarity of the background field. This magnetism is lost only if the rock is subsequently heated above a particular temperature (the Curie point which is 770 °C for iron). The magnetism left in rocks is a record of the magnetic field when the rock solidified.^[56]

Global map of magnetic anomalies Large craters and volcanoes are in dark green. Solid line represents the dichotomy boundary.

Chloride deposits

Using data from Mars Global Surveyor, Mars Odyssey and the Mars Reconnaissance Orbiter, scientists have found widespread deposits of chloride minerals. A picture below shows some deposits within the Phaethontis quadrangle. Evidence suggests that the deposits were formed from the evaporation of mineral enriched waters. The research suggests that lakes may have been scattered over large areas of the Martian surface. Usually chlorides are the last minerals to come out of solution. Carbonates, sulfates, and silica should precipitate out ahead of them. Sulfates and silica have been found by the Mars Rovers on the surface. Places with chloride minerals may have once held various life forms. Furthermore, such areas should preserve traces of ancient life.^[57]

Based on chloride deposits and hydrated phyllosilicates, Alfonso Davila and others believe there is an ancient lakebed in Terra Sirenum that had an area of 30,000 km² and was 200 meters deep. Other evidence that supports this lake are normal and inverted channels like ones found in the Atacama desert.^[58]

Evidence of water from chloride deposits in Phaethontis. Picture from HiRISE.

Fossae

The Elysium quadrangle is home to large troughs (long narrow depressions) called fossae in the geographical language used for Mars. Troughs are created when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano. Fossae/pit craters are common near volcanoes in the Tharsis and Elysium system of volcanoes.^[59]

Icaria Fossae Graben, as seen by HiRISE. Click on image for a better view of Dust Devil Tracks.

Sirenum Fossae Layers, as seen by HiRISE. Scale bar is 500 meters long.

Pits in troughs, as seen by HiRISE under HiWish program

Strange surfaces

Surface of crater floor, as seen by HiRISE under HiWish program.

Surface of crater floor showing details from image taken with HiRISE, under HiWish program. This may be a transition from one type of structure to a different, maybe due to erosion.

Surface showing large hollows of unknown origin, as seen by HiRISE under HiWish program.

Close-up of surface with large hollows, as seen by HiRISE under HiWish program.

Craters

Copernicus crater

The density of impact craters is used to determine the surface ages of Mars and other solar system bodies.^[60] The older the surface, the more craters present. Crater shapes can reveal the presence of ground ice.

MOLA image showing the relationship among Wright, Keeler, and Trumpler Craters. Colors indicate elevations.

East side of Hipparchus Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).

West side of Nansen Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).

The area around craters may be rich in minerals. On Mars, heat from the impact melts ice in the ground. Water from the melting ice dissolves minerals, and then deposits them in cracks or faults that were produced with the impact. This process, called hydrothermal alteration, is a major way in which ore deposits are produced. The area around Martian craters may be rich in useful ores for the future colonization of Mars.^[61]
Studies on the earth have documented that cracks are produced and that secondary minerals veins are deposited in the cracks.^[62]^[63]^[64] Images from satellites orbiting Mars have detected cracks near impact craters.^[65] Great amounts of heat are produced during impacts. The area around a large impact may take hundreds of thousands of years to cool.^[66]^[67]^[68]
Many craters once contained lakes.^[69]^[70]^[71] Because some crater floors show deltas, we know that water had to be present for some time. Dozens of deltas have been spotted on Mars.^[72] Deltas form when sediment is washed in from a stream entering a quiet body of water. It takes a bit of time to form a delta, so the presence of a delta is exciting; it means water was there for a time, maybe for many years. Primitive organisms may have developed in such lakes; hence, some craters may be prime targets for the search for evidence of life on the Red Planet.^[73]

List of craters

The following is a list of craters in the quadrangle. The crater's central location is of the quadrangle, craters that its central location is in another quadrangle is listed by eastern, western, northern or southern part.

Name	Location	Diameter	Year of approval
Avire	40°49′S 159°46′W / 40.82°S 159.76°W / -40.82; -159.76	6.85 km	2008
Belyov
Bunnik
Clark
Copernicus	48°48′S 168°48′W / 48.8°S 168.8°W / -48.8; -168.8	300 km	1973
Cross¹		Southern part
Dechu	42°15′S 157°59′W / 42.25°S 157.99°W / -42.25; -157.99	22 km	2018
Dokuchaev
Dunkassa
Eudoxus	44°54′S 147°30′W / 44.9°S 147.5°W / -44.9; -147.5	98 km	1973
Galap
Henbury
Hussey
Kamnik
Keeler	61°00′S 151°18′W / 61°S 151.3°W / -61; -151.3	95 km	1973
Koval'sky¹	Southern part	297 km¹	1973
Kuiper	57°24′S 157°18′W / 57.4°S 157.3°W / -57.4; -157.3	87 km	1973
Langtang
Li Fan	47°12′S 153°12′W / 47.2°S 153.2°W / -47.2; -153.2	104.8 km	1973
Liu Hsin	53°36′S 171°36′W / 53.6°S 171.6°W / -53.6; -171.6	137 km	1973
Magelhaens	32°22′S 194°41′W / 32.36°S 194.68°W / -32.36; -194.68	105 km
Mariner	35°06′S 164°30′W / 35.1°S 164.5°W / -35.1; -164.5	170 km	1967
Millman
Nansen	50°18′S 140°36′W / 50.3°S 140.6°W / -50.3; -140.6	81 km	1967
Naruko
Newton	40°48′S 158°06′W / 40.8°S 158.1°W / -40.8; -158.1	298 km	1973
Niquero
Nordenskiöld
Palikir	41°34′S 158°52′W / 41.57°S 158.86°W / -41.57; -158.86	15.57 km	2011
Pickering			1973
Ptolemaeus	48°13′S 157°36′W / 48.21°S 157.6°W / -48.21; -157.6	165 km	1973
Reutov
Selevac
Sitrah
Taltal
Triolet
Trumpler
Tyutaram			2013
Very	49°36′S 177°06′W / 49.6°S 177.1°W / -49.6; -177.1	114.8 km	1973
Wright	58°54′S 151°00′W / 58.9°S 151°W / -58.9; -151	113.7 km	1973
Yaren

¹Partly located in the quadrangle while another part is in a different quadrangle along with the crater's diameter

Mesa in a crater, as seen by HiRISE under HiWish program.

Layers in mantle, as seen by HiRISE under HiWish program.

Linear ridge networks

Linear ridge networks are found in various places on Mars in and around craters.^[74] Ridges often appear as mostly straight segments that intersect in a lattice-like manner. They are hundreds of meters long, tens of meters high, and several meters wide. It is thought that impacts created fractures in the surface, these fractures later acted as channels for fluids. Fluids cemented the structures. With the passage of time, surrounding material was eroded away, thereby leaving hard ridges behind.
Since the ridges occur in locations with clay, these formations could serve as a marker for clay which requires water for its formation.^[75]^[76]^[77] Water here could have supported past life in these locations. Clay may also preserve fossils or other traces of past life.

Linear ridge networks, as seen by HiRISE under HiWish program

Close-up of linear ridge networks from the previous image, as seen by HiRISE under HiWish program

Linear ridge networks, as seen by HiRISE under HiWish program

Linear ridge networks, as seen by HiRISE under HiWish program

Dunes

Sand dunes have been found in many places on Mars. The presence of dunes shows that the planet has an atmosphere with wind, for dunes require wind to pile up the sand. Most dunes on Mars are black because of the weathering of the volcanic rock basalt.^[78]^[79] Black sand can be found on Earth on Hawaii and on some tropical South Pacific islands.^[80]
Sand is common on Mars due to the old age of the surface that has allowed rocks to erode into sand. Dunes on Mars have been observed to move many meters.^[81]^[82]
Some dunes move along. In this process, sand moves up the windward side and then falls down the leeward side of the dune, thus caused the dune to go toward the leeward side (or slip face).^[83]
When images are enlarged, some dunes on Mars display ripples on their surfaces.^[84] These are caused by sand grains rolling and bouncing up the windward surface of a dune. The bouncing grains tend to land on the windward side of each ripple. The grains do not bounce very high so it does not take much to stop them.

Dunes in Newton (Martian crater), as seen by HiRISE under HiWish program

Close view of dunes in Newton Crater, as seen by HiRISE under HiWish program

Close view of dunes in Newton Crater, as seen by HiRISE under HiWish program

Close view of dunes in Newton Crater showing ripples on surface, as seen by HiRISE under HiWish program

Mantle

Much of the Martian surface is covered with a thick ice-rich, mantle layer that has fallen from the sky a number of times in the past.^[85]^[86]^[87] In some places a number of layers are visible in the mantle.^[88]

Tader Valles, as seen by THEMIS. Smooth material in channels may be a mantle in the form of dirty snow.

HiRISE image showing smooth mantle covering parts of a crater in the Phaethontis quadrangle. Along the outer rim of the crater, the mantle is displayed as layers. This suggests that the mantle was deposited multiple times in the past. Picture was taken with HiRISE under HiWish program. The layers are enlarged in the next image.

Enlargement of previous image of mantle layers. Four to five layers are visible. Location is the Phaethontis quadrangle.

Surface showing appearance with and without mantle covering, as seen by HiRISE, under the HiWish program Location is Terra Sirenum in Phaethontis quadrangle.

Surface appearance with and without mantle, as seen by HiRISE, under the HiWish program

Atlantis Chaos, within the Atlantis basin, as seen by HiRISE. Click on image to see mantle covering and possible gullies. The two images are different parts of the original image. They have different scales.

Channels

There is enormous evidence that water once flowed in river valleys on Mars.^[89]^[90] Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter.^[91]^[92]^[93]^[94] Indeed, a study published in June 2017, calculated that the volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had. Water was probably recycled many times from the ocean to rainfall around Mars.^[95]^[96]

Channel, as seen by HiRISE under HiWish program Streamlined shapes are indicated with arrows.

Oxbow lake, as seen by HiRISE under HiWish program

Channel connecting two craters, as seen by HiRISE under HiWish program

Channels, as seen by HiRISE under HiWish program

Channels, as seen by HiRISE under HiWish program

Other scenes in Phaethontis quadrangle

This topographic map shows volcanic peaks in white because of their great height. Near the equator, a line of three volcanoes points south to Phaethontis and three large craters-the area where there are many gullies. Click on the image for a good view.

Map of Phaethontis quadrangle. Click on to enlarge and see some crater names.

Close up image of Phaethontis surface taken with Mars Global Surveyor. Holes are thought to be caused by buried ice turning into a gas.

Pits on crater floor, as seen by HiRISE under HiWish program Pits may be formed when ice left the ground.ESP 050933 1355channel.jpg

Wide view of hollows, as seen by HiRISE under HiWish program Hollows may be formed as ice leaves the ground.

Close view of hollows, as seen by HiRISE under HiWish program

Close view of hollows, as seen by HiRISE under HiWish program

Other Mars quadrangles

0°N 180°W / 0°N 180°W / 0; -180

0°N 0°W / 0°N -0°E / 0; -0

90°N 0°W / 90°N -0°E / 90; -0

MC-01

Mare Boreum

MC-02

Diacria

MC-03

Arcadia

MC-04

Mare Acidalium

MC-05

Ismenius Lacus

MC-06

Casius

MC-07

Cebrenia

MC-08

Amazonis

MC-09

Tharsis

MC-10

Lunae Palus

MC-11

Oxia Palus

MC-12

Arabia

MC-13

Syrtis Major

MC-14

Amenthes

MC-15

Elysium

MC-16

Memnonia

MC-17

Phoenicis

MC-18

Coprates

MC-19

Margaritifer

MC-20

Sabaeus

MC-21

Iapygia

MC-22

Tyrrhenum

MC-23

Aeolis

MC-24

Phaethontis

MC-25

Thaumasia

MC-26

Argyre

MC-27

Noachis

MC-28

Hellas

MC-29

Eridania

MC-30

Mare Australe

The thirty cartographic quadrangles of Mars, defined by the United States Geological Survey.^[97]^[98] The quadrangles are numbered with the prefix "MC" for "Mars Chart."^[99] Click on a quadrangle name link and you will be taken to the corresponding article. North is at the top; 0°N 180°W / 0°N 180°W / 0; -180 is at the far left on the equator. The map images were taken by the Mars Global Surveyor.

[]

Interactive Mars map

Interactive imagemap of the global topography of Mars. Hover your mouse to see the names of over 25 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor. Reds and pinks are higher elevation (+3 km to +8 km); yellow is 0 km; greens and blues are lower elevation (down to −8 km). Whites (>+12 km) and browns (>+8 km) are the highest elevations. Axes are latitude and longitude; Poles are not shown.

(See also: Mars Rovers map) (view • discuss)

References

^ Davies, M.E.; Batson, R.M.; Wu, S.S.C. (1992). "Geodesy and Cartography". In Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; et al. Mars. Tucson: University of Arizona Press. ISBN 978-0-8165-1257-7..mw-parser-output cite.citation{font-style:inherit}.mw-parser-output q{quotes:"""""""'""'"}.mw-parser-output code.cs1-code{color:inherit;background:inherit;border:inherit;padding:inherit}.mw-parser-output .cs1-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-limited a,.mw-parser-output .cs1-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration{color:#555}.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration span{border-bottom:1px dotted;cursor:help}.mw-parser-output .cs1-hidden-error{display:none;font-size:100%}.mw-parser-output .cs1-visible-error{font-size:100%}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-right{padding-right:0.2em}

^ Blunck, J. 1982. Mars and its Satellites, Exposition Press. Smithtown, N.Y.

^ Murchie, S.; Mustard, John F.; Ehlmann, Bethany L.; Milliken, Ralph E.; et al. (2009). "A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter" (PDF). Journal of Geophysical Research. 114: E00D06. Bibcode:2009JGRE..11400D06M. doi:10.1029/2009JE003342.

^ Grant, J.; Wilson, Sharon A.; Noe Dobrea, Eldar; Fergason, Robin L.; et al. (2010). "HiRISE views enigmatic deposits in the Sirenum Fossae region of Mars". Icarus. 205: 53–63. Bibcode:2010Icar..205...53G. doi:10.1016/j.icarus.2009.04.009.

^ Kieffer, Hugh H. (1992). Mars. Tucson: University of Arizona Press. pp. ^{&#91, page&nbsp, needed&#93,}. ISBN 0-8165-1257-4.

^ https://www.uahirise.org/ESP_050948_1430

^ Irwin, Rossman P.; Howard, Alan D.; Maxwell, Ted A. (2004). "Geomorphology of Ma'adim Vallis, Mars, and associated paleolake basins". Journal of Geophysical Research. 109: 12009. Bibcode:2004JGRE..10912009I. doi:10.1029/2004JE002287.

^ Michael Carr (2006). The surface of Mars. Cambridge, UK: Cambridge University Press. pp. ^{&#91, page&nbsp, needed&#93,}. ISBN 0-521-87201-4.

^ Hartmann, W. (2003). A Traveler's Guide to Mars. New York: Workman Publishing. p. ^{[page needed]}. ISBN 978-0-7611-2606-5.

^ http://hirise.lpl.arizona.edu/PSP_004071_1425

^ http://hirise.lpl.arizona.edu/PSP_001948_1425

^ http://hirise.lpl.arizona.edu/PSP_004163_1375

^ U.S. department of the Interior U.S. Geological Survey, Topographic Map of the Eastern Region of Mars M 15M 0/270 2AT, 1991

^ Edgett, K.; Malin, M. C.; Williams, R. M. E.; Davis, S. D. (2003). "Polar-and middle-latitude martian gullies: A view from MGS MOC after 2 Mars years in the mapping orbit" (PDF). Lunar Planet. Sci. 34. p. 1038, Abstract 1038. Bibcode:2003LPI....34.1038E.

^ ^a^b Dickson, J; Head, J; Kreslavsky, M (2007). "Martian gullies in the southern mid-latitudes of Mars: Evidence for climate-controlled formation of young fluvial features based upon local and global topography" (PDF). Icarus. 188 (2): 315–323. Bibcode:2007Icar..188..315D. doi:10.1016/j.icarus.2006.11.020.

^ http://www.psrd.hawaii.edu/Aug03/MartianGullies.html

^ ^a^b Heldmann, J; Mellon, Michael T (2004). "Observations of martian gullies and constraints on potential formation mechanisms". Icarus. 168 (2): 285–304. Bibcode:2004Icar..168..285H. doi:10.1016/j.icarus.2003.11.024.

^ Forget, F. et al. 2006. Planet Mars Story of Another World. Praxis Publishing. Chichester, UK.

^ http://www.space.com/scienceastronomy/mars_aquifer_041112.html

^ Harris, A and E. Tuttle. 1990. Geology of National Parks. Kendall/Hunt Publishing Company. Dubuque, Iowa

^ Malin, Michael C.; Edgett, Kenneth S. (2001). "Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission". Journal of Geophysical Research. 106: 23429–23570. Bibcode:2001JGR...10623429M. doi:10.1029/2000JE001455.

^ Mustard, JF; Cooper, CD; Rifkin, MK (2001). "Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice" (PDF). Nature. 412 (6845): 411–4. doi:10.1038/35086515. PMID 11473309.

^ Carr, Michael H. (2001). "Mars Global Surveyor observations of Martian fretted terrain". Journal of Geophysical Research. 106: 23571–23595. Bibcode:2001JGR...10623571C. doi:10.1029/2000JE001316.

^ http://www.msnbc.msn.com/id/15702457?

^ Head, J. W.; Marchant, D. R.; Kreslavsky, M. A. (2008). "From the Cover: Formation of gullies on Mars: Link to recent climate history and insolation microenvironments implicate surface water flow origin". Proceedings of the National Academy of Sciences. 105 (36): 13258–63. Bibcode:2008PNAS..10513258H. doi:10.1073/pnas.0803760105. PMC 2734344. PMID 18725636.

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^ http://news.nationalgeographic.com/news/2008/03/080319-mars-gullies_2.html

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^ Langlais, B. (2004). "Crustal magnetic field of Mars" (PDF). Journal of Geophysical Research. 109. Bibcode:2004JGRE..10902008L. doi:10.1029/2003JE002048.
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^ Connerney, J. E. P.; Acuña, MH; Ness, NF; Kletetschka, G; et al. (2005). "Tectonic implications of Mars crustal magnetism". Proceedings of the National Academy of Sciences. 102 (42): 14970–14975. Bibcode:2005PNAS..10214970C. doi:10.1073/pnas.0507469102. PMC 1250232. PMID 16217034.

^ Acuna, MH; Connerney, JE; Ness, NF; Lin, RP; Mitchell, D; Carlson, CW; McFadden, J; Anderson, KA; et al. (1999). "Global distribution of crustal magnetization discovered by the Mars Global Surveyor MAG/ER Experiment". Science. 284 (5415): 790–793. Bibcode:1999Sci...284..790A. doi:10.1126/science.284.5415.790. PMID 10221908.

^ http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=31028&fbodylongid=645

^ Osterloo, M. M.; Hamilton, V. E.; Bandfield, J. L.; Glotch, T. D.; et al. (2008). "Chloride-Bearing Materials in the Southern Highlands of Mars". Science. 319 (5870): 1651–1654. Bibcode:2008Sci...319.1651O. doi:10.1126/science.1150690. PMID 18356522.

^ Davila, A.; et al. (2011). "A large sedimentary basin in the Terra Sirenum region of the southern highlands of Mars". Icarus. 212: 579–589. Bibcode:2011Icar..212..579D. doi:10.1016/j.icarus.2010.12.023.CS1 maint: Explicit use of et al. (link)

^ Skinner, J., L. Skinner, and J. Kargel. 2007. Re-assessment of Hydrovolcanism-based Resurfacing within the Galaxias Fossae Region of Mars. Lunar and Planetary Science XXXVIII (2007)

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^ Osinski, G, J. Spray, and P. Lee. 2001. Impact-induced hydrothermal activity within the Haughton impact structure, arctic Canada: Generation of a transient, warm, wet oasis. Meteoritics & Planetary Science: 36. 731-745

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^ Head, J. and J. Mustard. 2006. Breccia Dikes and Crater-Related Faults in Impact Craters on Mars: Erosion and Exposure on the Floor of a 75-km Diameter Crater at the Dichotomy Boundary. Special Issue on Role of Volatiles and Atmospheres on Martian Impact Craters Meteoritics & Planetary Science

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^ Mustard, J., et al. 2001. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice. Nature 412 (6845), 411–414.

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External links

General review of many of the theories involving the origin of gullies.

Dickson, J; Head, J; Kreslavsky, M (2007). "Martian gullies in the southern mid-latitudes of Mars: Evidence for climate-controlled formation of young fluvial features based upon local and global topography" (PDF). Icarus. 188 (2): 315–323. Bibcode:2007Icar..188..315D. doi:10.1016/j.icarus.2006.11.020. Gives a good review of the history of the discovery of gullies.

Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention

[1] Davies, M.E.; Batson, R.M.; Wu, S.S.C. (1992). "Geodesy and Cartography". In Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; et al. Mars. Tucson: University of Arizona Press. ISBN 978-0-8165-1257-7..mw-parser-output cite.citation{font-style:inherit}.mw-parser-output q{quotes:"""""""'""'"}.mw-parser-output code.cs1-code{color:inherit;background:inherit;border:inherit;padding:inherit}.mw-parser-output .cs1-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-limited a,.mw-parser-output .cs1-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration{color:#555}.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration span{border-bottom:1px dotted;cursor:help}.mw-parser-output .cs1-hidden-error{display:none;font-size:100%}.mw-parser-output .cs1-visible-error{font-size:100%}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-right{padding-right:0.2em}

[2] Blunck, J. 1982. Mars and its Satellites, Exposition Press. Smithtown, N.Y.

[3] Murchie, S.; Mustard, John F.; Ehlmann, Bethany L.; Milliken, Ralph E.; et al. (2009). "A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter" (PDF). Journal of Geophysical Research. 114: E00D06. Bibcode:2009JGRE..11400D06M. doi:10.1029/2009JE003342.

[4] Grant, J.; Wilson, Sharon A.; Noe Dobrea, Eldar; Fergason, Robin L.; et al. (2010). "HiRISE views enigmatic deposits in the Sirenum Fossae region of Mars". Icarus. 205: 53–63. Bibcode:2010Icar..205...53G. doi:10.1016/j.icarus.2009.04.009.

[5] Kieffer, Hugh H. (1992). Mars. Tucson: University of Arizona Press. pp. ^{&#91, page&nbsp, needed&#93,}. ISBN 0-8165-1257-4.

[6] ttps://www.uahirise.org/ESP_050948_1430

[7] Irwin, Rossman P.; Howard, Alan D.; Maxwell, Ted A. (2004). "Geomorphology of Ma'adim Vallis, Mars, and associated paleolake basins". Journal of Geophysical Research. 109: 12009. Bibcode:2004JGRE..10912009I. doi:10.1029/2004JE002287.

[8] Michael Carr (2006). The surface of Mars. Cambridge, UK: Cambridge University Press. pp. ^{&#91, page&nbsp, needed&#93,}. ISBN 0-521-87201-4.

[9] Hartmann, W. (2003). A Traveler's Guide to Mars. New York: Workman Publishing. p. ^{[page needed]}. ISBN 978-0-7611-2606-5.

[10] ttp://hirise.lpl.arizona.edu/PSP_004071_1425

[11] ttp://hirise.lpl.arizona.edu/PSP_001948_1425

[12] ttp://hirise.lpl.arizona.edu/PSP_004163_1375

[13] U.S. department of the Interior U.S. Geological Survey, Topographic Map of the Eastern Region of Mars M 15M 0/270 2AT, 1991

[14] Edgett, K.; Malin, M. C.; Williams, R. M. E.; Davis, S. D. (2003). "Polar-and middle-latitude martian gullies: A view from MGS MOC after 2 Mars years in the mapping orbit" (PDF). Lunar Planet. Sci. 34. p. 1038, Abstract 1038. Bibcode:2003LPI....34.1038E.

[2007Icar..188..315D-15] Dickson, J; Head, J; Kreslavsky, M (2007). "Martian gullies in the southern mid-latitudes of Mars: Evidence for climate-controlled formation of young fluvial features based upon local and global topography" (PDF). Icarus. 188 (2): 315–323. Bibcode:2007Icar..188..315D. doi:10.1016/j.icarus.2006.11.020.

[16] ttp://www.psrd.hawaii.edu/Aug03/MartianGullies.html

[Heldmann_2004-17] Heldmann, J; Mellon, Michael T (2004). "Observations of martian gullies and constraints on potential formation mechanisms". Icarus. 168 (2): 285–304. Bibcode:2004Icar..168..285H. doi:10.1016/j.icarus.2003.11.024.

[18] Forget, F. et al. 2006. Planet Mars Story of Another World. Praxis Publishing. Chichester, UK.

[19] ttp://www.space.com/scienceastronomy/mars_aquifer_041112.html

[20] Harris, A and E. Tuttle. 1990. Geology of National Parks. Kendall/Hunt Publishing Company. Dubuque, Iowa

[21] Malin, Michael C.; Edgett, Kenneth S. (2001). "Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission". Journal of Geophysical Research. 106: 23429–23570. Bibcode:2001JGR...10623429M. doi:10.1029/2000JE001455.

[22] Mustard, JF; Cooper, CD; Rifkin, MK (2001). "Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice" (PDF). Nature. 412 (6845): 411–4. doi:10.1038/35086515. PMID 11473309.

[23] Carr, Michael H. (2001). "Mars Global Surveyor observations of Martian fretted terrain". Journal of Geophysical Research. 106: 23571–23595. Bibcode:2001JGR...10623571C. doi:10.1029/2000JE001316.

[24] ttp://www.msnbc.msn.com/id/15702457?

[25] Head, J. W.; Marchant, D. R.; Kreslavsky, M. A. (2008). "From the Cover: Formation of gullies on Mars: Link to recent climate history and insolation microenvironments implicate surface water flow origin". Proceedings of the National Academy of Sciences. 105 (36): 13258–63. Bibcode:2008PNAS..10513258H. doi:10.1073/pnas.0803760105. PMC 2734344. PMID 18725636.

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