Protonilus Mensae is an area of

Mars Mars is the fourth planet from the Sun. It is also known as the "Red Planet", because of its orange-red appearance. Mars is a desert-like rocky planet with a tenuous carbon dioxide () atmosphere. At the average surface level the atmosph ...

in the

Ismenius Lacus quadrangle The Ismenius Lacus quadrangle is one of a series of list of quadrangles on Mars, 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Quadrangle (geography), quadrangle is located in th ...

. It is centered on the coordinates of 43.86° N and 49.4° E. Its western and eastern longitudes are 37° E and 59.7° E. North and south latitudes are 47.06° N and 39.87° N. Protonilus Mensae is between Deuteronilus Mensae and Nilosyrtis Mensae; all lie along the Martian dichotomy boundary. Its name was adapted by the IAU in 1973. Mapdeuteronilus.jpg, Map showing the relation of Protonilus and Deuteronilus Mensae to other nearby regions. Colors refer to altitudes. The surface is described as

fretted terrain Fretted terrain is a type of surface feature common to certain areas of Mars and was discovered in Mariner 9 images. It lies between two different types of terrain. The surface of Mars can be divided Martian dichotomy, into two parts: low, young, ...

. This terrain contains cliffs, mesas, and wide flat valleys. Surface features are believed to have been caused by debris-covered glaciers.NASA.gov
/ref> These glaciers are termed lobate debris aprons (LDA) when surrounding mounds and mesas. When glaciers are in valleys, they are called Lineated valley fill (LVF). Parts of the surface show flow patterns that start in numerous alcoves located within the walls of plateaus. Small flow lobes on top of main flows demonstrate that there was more than one glacial period, just as on Earth. It is strongly believed that beneath a thin layer of rock and dust lie vast reservoirs of ice. Radar data from the SHAllow RADar (SHARAD) on board MRO have found pure ice under LDA and LVF. Some places in Protonilus Mensae display lines of pits. These pits may have formed when ground ice converted to a gas, thus leaving a void. When surface material collapses into voids, pits are created.

Dunes

ESP 044861 2225dunes.jpg, Wide view of dunes in Moreux Crater, as seen by HiRISE under HiWish program 44861 2225dunesbottom.jpg, Enlarged view of dunes on the bottom of the previous image, as seen by HiRISE under HiWish program 44861 2225duneclose.jpg, Close view of one large dune from the same location, as seen by HiRISE under HiWish program 44861 2225dunesclose.jpg, Close view of white spot among the dark dunes showing ripples and streaks

Climate change caused ice-rich features

Many features on Mars, including ones in Protonilus Mensae, are believed to contain large amounts of ice. The most popular model for the origin of the ice is climate change from large changes in the tilt of the planet's rotational axis. At times the tilt has even been greater than 80 degrees Large changes in the tilt explains many ice-rich features on Mars. Studies have shown that when the tilt of Mars reaches 45 degrees from its current 25 degrees, ice is no longer stable at the poles. Furthermore, at this high tilt, stores of solid carbon dioxide (dry ice) sublimate, thereby increasing the atmospheric pressure. This increased pressure allows more dust to be held in the atmosphere. Moisture in the atmosphere will fall as snow or as ice frozen onto dust grains. Calculations suggest this material will concentrate in the mid-latitudes. General circulation models of the Martian atmosphere predict accumulations of ice-rich dust in the same areas where ice-rich features are found. When the tilt begins to return to lower values, the ice sublimates (turns directly to a gas) and leaves behind a lag of dust.Mellon, M., B. Jakosky. 1995. The distribution and behavior of Martian ground ice during past and present epochs. J. Geophys. Res. 100, 11781–11799. The lag deposit caps the underlying material so with each cycle of high tilt levels, some ice-rich mantle remains behind.Madeleine, J., F. Forget, J. Head, B. Levrard, F. Montmessin. 2007. Exploring the northern mid-latitude glaciation with a general circulation model. In: Seventh International Conference on Mars. Abstract 3096. Note, that the smooth surface mantle layer probably represents only relative recent material.

Brain terrain

Brain terrain is a region of maze-like ridges 3–5 meters high. Some ridges may consist of an ice core, so they may be sources of water for future colonists.Levy, J., J. Head, D. Marchant. 2009. Concentric crater fill in Utopia Planitia: History and interaction between glacial “brain terrain” and periglacial mantle processes. Icarus 202, 462–476. ESP 045349 2235brains.jpg, Wide view of brain terrain being formed, as seen by HiRISE under HiWish program 45349 2235brainsforming4.jpg, Brain terrain being formed, as seen by HiRISE under HiWish program Note: this is an enlargement of previous image using HiView. 45349 2235brainsforming3.jpg, Brain terrain being formed, as seen by HiRISE under HiWish program Note: this is an enlargement of a previous image using HiView. 45349 2235brainsforming2.jpg, Brain terrain being formed, as seen by HiRISE under HiWish program Note: this is an enlargement of a previous image using HiView. Arrows indicate spots where brain terrain is beginning to form. 45349 2235brainsforming.jpg, Brain terrain being formed, as seen by HiRISE under HiWish program Note: this is an enlargement of a previous image using HiView. Arrows indicate spots where brain terrain is beginning to form. 45349 2235brainschanging.jpg, Brain terrain being formed, as seen by HiRISE under HiWish program Note: this is an enlargement of a previous image using HiView.

Glaciers

Image:Glacier as seen by ctx.JPG, Mesa in

, as seen by CTX. Mesa has several glaciers eroding it. One of the glaciers is seen in greater detail in the next two images from HiRISE. Image:Wide view of glacier showing image field.JPG, Glacier as seen by HiRISE under the HiWish program. Area in rectangle is enlarged in the next photo. Zone of accumulation of snow at the top. Glacier is moving down valley, then spreading out on plain. Evidence for flow comes from the many lines on surface. Location is in Protonilus Mensae in

. Image:Glacier close up with hirise.JPG, Enlargement of area in rectangle of the previous image. On Earth the ridge would be called the terminal moraine of an alpine glacier. Picture taken with HiRISE under the HiWish program. Image:CTX Context Image of Pits.JPG, CTX Image in Protonilus Mensae, showing location of next image. Image:Pits in Protonilus Mensae.JPG, Pits in Protonilus Mensae, as seen by HiRISE, under the

HiWish program HiWish is a program created by NASA so that anyone can suggest a place for the HiRISE camera on the Mars Reconnaissance Orbiter to photograph. It was started in January 2010. In the first few months of the program 3000 people signed up to use HiR ...

. Image:25305glacierend.jpg, End of a glacier, as seen by HiRISE under HiWish program. Surface to the right of the end moraine exhibits patterned ground, which is common where ground water has frozen. Image:25305roughsurface.jpg, Surface forms in Ismenius Lacus, as seen by HiRISE under HiWish program. Wikifrettedctxp22.jpg, Wide CTX view showing mesa and buttes with Lobate debris aprons and lineated valley fill around them. Location is

. WikiESP 020769 2225fretted.jpg, Close-up of lineated valley fill (LVF), as seen by HiRISE under HiWish program. Note: this is an enlargement of the previous CTX image. ESP 044874 2205glaciers.jpg, Glaciers moving in two different valleys, as seen by HiRISE under HiWish program

References

{{Portal bar, Solar System Ismenius Lacus quadrangle Mensae on Mars

Dunes

Climate change caused ice-rich features

Brain terrain

Glaciers

See also

References