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Cuadrángulo del Lago Ismenius

Imagen del Cuadrángulo del Lago Ismenius (MC-5). La zona norte contiene llanuras relativamente suaves; la zona central, mesetas y cerros; y la zona sur, numerosos cráteres.

El cuadrángulo Ismenius Lacus es uno de una serie de 30 mapas cuadrangulares de Marte utilizados por el Programa de Investigación de Astrogeología del Servicio Geológico de los Estados Unidos (USGS) . El cuadrángulo está ubicado en la porción noroeste del hemisferio oriental de Marte y cubre de 0° a 60° de longitud este (300° a 360° de longitud oeste) y de 30° a 65° de latitud norte. El cuadrángulo utiliza una proyección cónica conforme de Lambert a una escala nominal de 1:5 000 000 (1:5M). El cuadrángulo Ismenius Lacus también se conoce como MC-5 (Mars Chart-5). [1] Los límites sur y norte del cuadrángulo Ismenius Lacus tienen aproximadamente 3065 km (1905 mi) y 1500 km (930 mi) de ancho, respectivamente. La distancia de norte a sur es de unos 2050 km (1270 mi) (un poco menos que la longitud de Groenlandia). [2] El cuadrángulo cubre un área aproximada de 4,9 millones de kilómetros cuadrados, o un poco más del 3% de la superficie de Marte. [3] El cuadrángulo de Ismenius Lacus contiene partes de Acidalia Planitia , Arabia Terra , Vastitas Borealis y Terra Sabaea . [4]

El cuadrángulo de Ismenius Lacus contiene Deuteronilus Mensae y Protonilus Mensae , dos lugares que son de especial interés para los científicos. Contienen evidencia de actividad glacial presente y pasada. También tienen un paisaje único en Marte, llamado terreno erosionado . El cráter más grande del área es el cráter Lyot , que contiene canales probablemente tallados por agua líquida. [5] [6]

Origen de los nombres

Cadmo mata al dragón de la primavera de Ismenia

Ismenius Lacus es el nombre de una formación de albedo telescópica situada a 40° N y 30° E en Marte. El término en latín significa lago Ismenio y se refiere al manantial Ismenio cerca de Tebas en Grecia, donde Cadmo mató al dragón guardián. Cadmo fue el legendario fundador de Tebas y había ido al manantial para buscar agua. El nombre fue aprobado por la Unión Astronómica Internacional (UAI) en 1958. [7]

En esta región parecía haber un gran canal llamado Nilo. Desde 1881-1882 se dividió en otros canales, algunos de los cuales se denominaron Nilosyrtis, Protonilus (primer Nilo) y Deuteronilus (segundo Nilo). [8]

Fisiografía y geología

En el este del lago Ismenius, se encuentra Mamers Valles , un canal de salida gigante.

El canal que se muestra a continuación recorre una gran distancia y tiene ramificaciones. Termina en una depresión que puede haber sido un lago en algún momento. La primera imagen es un gran angular, tomada con CTX; mientras que la segunda es un primer plano tomado con HiRISE. [9]

Cráter Lyot

Las llanuras del norte son generalmente planas y lisas con pocos cráteres. Sin embargo, algunos cráteres grandes se destacan. El cráter de impacto gigante , Lyot, es fácil de ver en la parte norte de Ismenius Lacus. [10] El cráter Lyot es el punto más profundo del hemisferio norte de Marte. [11] Una imagen a continuación de las dunas del cráter Lyot muestra una variedad de formas interesantes: dunas oscuras, depósitos de tonos claros y rastros de remolinos de polvo . Los remolinos de polvo, que se parecen a tornados en miniatura, crean los rastros al eliminar un depósito delgado pero brillante de polvo para revelar la superficie subyacente más oscura. Se cree ampliamente que los depósitos de tonos claros contienen minerales formados en agua. Una investigación, publicada en junio de 2010, describió evidencia de agua líquida en el cráter Lyot en el pasado. [5] [6]

Se han encontrado muchos canales cerca del cráter Lyot. Una investigación, publicada en 2017, concluyó que los canales se formaron a partir del agua liberada cuando el material eyectado caliente aterrizó en una capa de hielo de entre 20 y 300 metros de espesor. Los cálculos sugieren que el material eyectado habría tenido una temperatura de al menos 250 grados Fahrenheit. Los valles parecen comenzar debajo del material eyectado cerca del borde exterior del mismo. Una evidencia de esta idea es que hay pocos cráteres secundarios cerca. Pocos cráteres secundarios se formaron porque la mayoría aterrizó en el hielo y no afectó al suelo de abajo. El hielo se acumuló en el área cuando el clima era diferente. La inclinación u oblicuidad del eje cambia con frecuencia. Durante los períodos de mayor inclinación, el hielo de los polos se redistribuye a las latitudes medias. La existencia de estos canales es inusual porque, aunque Marte solía tener agua en ríos, lagos y un océano, estas características se han datado en los períodos Noéico y Hespériense , hace 4 a 3 mil millones de años. [12] [13] [14]

Otros cráteres

Los cráteres de impacto suelen tener un borde con material eyectado a su alrededor; en cambio, los cráteres volcánicos no suelen tener borde ni depósitos de material eyectado. A medida que los cráteres se hacen más grandes (superiores a 10 km de diámetro), suelen tener un pico central. [15] El pico se produce por un rebote del suelo del cráter tras el impacto. [16] A veces, los cráteres muestran capas en sus paredes. Dado que la colisión que produce un cráter es como una potente explosión, las rocas de las profundidades subterráneas son arrojadas a la superficie. Por lo tanto, los cráteres son útiles para mostrarnos lo que se encuentra en las profundidades de la superficie.

Terreno accidentado

El cuadrángulo de Ismenius Lacus contiene varias características interesantes, como el terreno erosionado , partes del cual se encuentran en Deuteronilus Mensae y Protonilus Mensae. El terreno erosionado contiene tierras bajas lisas y planas junto con acantilados escarpados. Las escarpaduras o acantilados suelen tener entre 1 y 2 km de altura. Los canales de la zona tienen suelos anchos y planos y paredes escarpadas. Hay muchos montículos y mesetas . En el terreno erosionado, la tierra parece pasar de valles estrechos y rectos a mesetas aisladas. [19] La mayoría de las mesetas están rodeadas de formas que han recibido una variedad de nombres: delantales circunmesa, delantales de escombros, glaciares de roca y delantales de escombros lobulados . [20] Al principio parecían parecerse a los glaciares de roca de la Tierra. Pero los científicos no podían estar seguros. Incluso después de que la cámara Mars Orbiter Camera (MOC) del Mars Global Surveyor (MGS) tomara diversas fotografías del terreno irregular, los expertos no podían decir con certeza si el material se movía o fluía como lo haría en un depósito rico en hielo (glaciar). Finalmente, los estudios de radar con el Mars Reconnaissance Orbiter descubrieron pruebas de su verdadera naturaleza , que mostraron que contienen hielo de agua puro cubierto con una fina capa de rocas que aislaban el hielo. [21] [22]

Glaciares

Los glaciares formaron gran parte de la superficie observable en grandes áreas de Marte. Se cree que gran parte del área en latitudes altas, especialmente el cuadrángulo Ismenius Lacus, aún contiene enormes cantidades de hielo de agua. [16] [21] [23] En marzo de 2010, los científicos publicaron los resultados de un estudio de radar de un área llamada Deuteronilus Mensae que encontró evidencia generalizada de hielo debajo de unos pocos metros de escombros de roca. [24] El hielo probablemente se depositó como nevada durante un clima anterior cuando los polos estaban más inclinados. [25] Sería difícil hacer una caminata en el terreno erosionado donde los glaciares son comunes porque la superficie está plegada, picada y a menudo cubierta con estrías lineales. [26] Las estrías muestran la dirección del movimiento. Gran parte de esta textura rugosa se debe a la sublimación del hielo enterrado. El hielo se convierte directamente en gas (este proceso se llama sublimación) y deja atrás un espacio vacío. El material superpuesto luego colapsa en el vacío. [27] Los glaciares no son hielo puro; contienen tierra y rocas. A veces, vierten su carga de materiales en crestas. Estas crestas se llaman morrenas . Algunos lugares en Marte tienen grupos de crestas que están retorcidas; esto puede haberse debido a un mayor movimiento después de que se formaron las crestas. A veces, trozos de hielo caen del glaciar y quedan enterrados en la superficie terrestre. Cuando se derriten, queda un agujero más o menos redondo. [28] En la Tierra llamamos a estas características calderas o agujeros de caldera. El parque Mendon Ponds en el norte del estado de Nueva York ha preservado varias de estas calderas. La imagen de HiRISE a continuación muestra posibles calderas en el cráter Moreux.

Latitude dependent 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.[29][30][31]

Climate change caused ice-rich features

Many features on Mars, especially ones found in the Ismenius Lacus quadrangle, 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[32][33] 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.[34] 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.[35][36] General circulation models of the Martian atmosphere predict accumulations of ice-rich dust in the same areas where ice-rich features are found.[33] When the tilt begins to return to lower values, the ice sublimates (turns directly to a gas) and leaves behind a lag of dust.[37][38] The lag deposit caps the underlying material so with each cycle of high tilt levels, some ice-rich mantle remains behind.[39] Note that the smooth surface mantle layer probably represents only relative recent material.

Upper Plains Unit

Remnants of a 50–100 meter thick mantling, called the Upper Plains Unit, has been discovered in the mid-latitudes of Mars. First investigated in the Deuteronilus Mensae region, but it occurs in other places as well. The remnants consist of sets of dipping layers in craters and along mesas.[40][41] Sets of dipping layers may be of various sizes and shapes—some look like Aztec pyramids from Central America.

This unit also degrades into 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.

Some regions of the upper plains unit display large fractures and troughs with raised rims; such regions are called ribbed upper plains. Fractures are believed to have started with small cracks from stresses. Stress is suggested to initiate the fracture process since ribbed upper plains are common when debris aprons come together or near the edge of debris aprons—such sites would generate compressional stresses. Cracks exposed more surfaces, and consequently more ice in the material sublimates into the planet's thin atmosphere. Eventually, small cracks become large canyons or troughs.

Small cracks often contain small pits and chains of pits; these are thought to be from sublimation of ice in the ground.[42][43] Large areas of the Martian surface are loaded with ice that is protected by a meters thick layer of dust and other material. However, if cracks appear, a fresh surface will expose ice to the thin atmosphere.[44][45] In a short time, the ice will disappear into the cold, thin atmosphere in a process called sublimation. Dry ice behaves in a similar fashion on the Earth. On Mars sublimation has been observed when the Phoenix lander uncovered chunks of ice that disappeared in a few days.[46][47] In addition, HiRISE has seen fresh craters with ice at the bottom. After a time, HiRISE saw the ice deposit disappear.[48]

The upper plains unit is thought to have fallen from the sky. It drapes various surfaces, as if it fell evenly. As is the case for other mantle deposits, the upper plains unit has layers, is fine-grained, and is ice-rich. It is widespread; it does not seem to have a point source. The surface appearance of some regions of Mars is due to how this unit has degraded. It is a major cause of the surface appearance of lobate debris aprons.[43] The layering of the upper plains mantling unit and other mantling units are believed to be caused by major changes in the planet's climate. Models predict that the obliquity or tilt of the rotational axis has varied from its present 25 degrees to maybe over 80 degrees over geological time. Periods of high tilt will cause the ice in the polar caps to be redistributed and change the amount of dust in the atmosphere.[50][51][52]

Dipping layers

In many locations around Mars are features that have been called "dipping layers" These features are groups of layers in protected place like inside of craters or against slopes. Although they once covered a wide area, today they exist only in certain spots because erosion has removed most of the material. Several ideas have been advanced for how they were formed.[53] The material that formed them may have dropped from the sky as ice-rich dust.[54] [55] [56] Another idea for their origin was presented at 55th LPSC (2024) by an international team of researchers. They suggest that the layers are from past ice sheets.[57]

Deltas

Researchers have found a number of examples of deltas that formed in Martian lakes. Deltas are major signs that Mars once had a lot of water because deltas usually require deep water over a long period of time to form. In addition, the water level needs to be stable to keep sediment from washing away. Deltas have been found over a wide geographical range. Below, is a pictures of a one in the Ismenius Lacus quadrangle.[58]

Pits and cracks

Some places in the Ismenius Lacus quadrangle display large numbers of cracks and pits. It is widely believed that these are the result of ground ice sublimating (changing directly from a solid to a gas). After the ice leaves, the ground collapses in the shape of pits and cracks. The pits may come first. When enough pits form, they unite to form cracks.[59]

Mesas formed by ground collapse

Volcanoes under ice

There is evidence that volcanoes sometimes erupt under ice, as they do on Earth at times. What seems to happen it that much ice melts, the water escapes, and then the surface cracks and collapses.[60] These exhibit concentric fractures and large pieces of ground that seemed to have been pulled apart. Sites like this may have recently had held liquid water, hence they may be fruitful places to search for evidence of life.[61][62]

Exhumed craters

Some features on Mars seem to be in the process of being uncovered. So, the thought is that they formed, were covered over, and now are being exhumed as material is being eroded. These features are quite noticeable with craters. When a crater forms, it will destroy what is under it and leave a rim and ejecta. In the example below, only part of the crater is visible. if the crater came after the layered feature, it would have removed part of the feature.

Fractures forming blocks

In places large fractures break up surfaces. Sometimes straight edges are formed and large cubes are created by the fractures.

Polygonal patterned ground

Polygonal, patterned ground is quite common in some regions of Mars.[63][64][65][66][67][68][69] It is commonly believed to be caused by the sublimation of ice from the ground. Sublimation is the direct change of solid ice to a gas. This is similar to what happens to dry ice on the Earth. Places on Mars that display polygonal ground may indicate where future colonists can find water ice. Patterned ground forms in a mantle layer, called latitude dependent mantle, that fell from the sky when the climate was different.[29][30][70][71]

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.[72][73] Black sand can be found on Earth on Hawaii and on some tropical South Pacific islands.[74]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.[75][76]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).[77]When images are enlarged, some dunes on Mars display ripples on their surfaces.[78] 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.

Ocean

Many researchers have suggested that Mars once had a great ocean in the north.[79][80][81][82][83][84][85] Much evidence for this ocean has been gathered over several decades. New evidence was published in May 2016. A large team of scientists described how some of the surface in Ismenius Lacus quadrangle was altered by two tsunamis. The tsunamis were caused by asteroids striking the ocean. Both were thought to have been strong enough to create 30 km diameter craters. The first tsunami picked up and carried boulders the size of cars or small houses. The backwash from the wave formed channels by rearranging the boulders. The second came in when the ocean was 300 m lower. The second carried a great deal of ice which was dropped in valleys. Calculations show that the average height of the waves would have been 50 m, but the heights would vary from 10 m to 120 m. Numerical simulations show that in this particular part of the ocean two impact craters of the size of 30 km in diameter would form every 30 million years. The implication here is that a great northern ocean may have existed for millions of years. One argument against an ocean has been the lack of shoreline features. These features may have been washed away by these tsunami events. The parts of Mars studied in this research are Chryse Planitia and northwestern Arabia Terra. These tsunamis affected some surfaces in the Ismenius Lacus quadrangle and in the Mare Acidalium quadrangle.[86][87][88][89]

Gullies

Gullies were thought for a time to have been caused by recent flows of liquid water. However, further study suggests they are formed today by chunks of dry ice moving down steep slopes.[90]

Layered features

Ring mold craters

Ring Mold Craters are a kind of crater on the planet Mars, that look like the ring molds used in baking. They are believed to be caused by an impact into ice. The ice is covered by a layer of debris. They are found in parts of Mars that have buried ice. Laboratory experiments confirm that impacts into ice result in a "ring mold shape." They are also bigger than other craters in which an asteroid impacted solid rock. Impacts into ice warm the ice and cause it to flow into the ring mold shape.

However, another idea for their formation has emerged.[91]The other idea for their formation revolves around the impacting body going through layers of different densities. Later erosion could have helped shape them. It was thought that ring-mold craters could only exist in areas with large amounts of ground ice. However, with more extensive analysis of larger areas, it was found the ring mold craters are sometimes formed where there is not as much ice underground.[92] [93]

Mounds

Channels

Landslide

Other images

Other Mars quadrangles

Interactive Mars map

Map of MarsAcheron FossaeAcidalia PlanitiaAlba MonsAmazonis PlanitiaAonia PlanitiaArabia TerraArcadia PlanitiaArgentea PlanumArgyre PlanitiaChryse PlanitiaClaritas FossaeCydonia MensaeDaedalia PlanumElysium MonsElysium PlanitiaGale craterHadriaca PateraHellas MontesHellas PlanitiaHesperia PlanumHolden craterIcaria PlanumIsidis PlanitiaJezero craterLomonosov craterLucus PlanumLycus SulciLyot craterLunae PlanumMalea PlanumMaraldi craterMareotis FossaeMareotis TempeMargaritifer TerraMie craterMilankovič craterNepenthes MensaeNereidum MontesNilosyrtis MensaeNoachis TerraOlympica FossaeOlympus MonsPlanum AustralePromethei TerraProtonilus MensaeSirenumSisyphi PlanumSolis PlanumSyria PlanumTantalus FossaeTempe TerraTerra CimmeriaTerra SabaeaTerra SirenumTharsis MontesTractus CatenaTyrrhena TerraUlysses PateraUranius PateraUtopia PlanitiaValles MarinerisVastitas BorealisXanthe Terra
The image above contains clickable linksInteractive image map of the global topography of Mars. Hover your mouse over the image to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor. Whites and browns indicate the highest elevations (+12 to +8 km); followed by pinks and reds (+8 to +3 km); yellow is 0 km; greens and blues are lower elevations (down to −8 km). Axes are latitude and longitude; Polar regions are noted.
(See also: Mars Rovers map and Mars Memorial map) (view • discuss)


See also

References

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