Hale (Martian crater)

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Hale
Planet Mars
Coordinates 35°42′S 323°24′E / 35.7°S 323.4°E / -35.7; 323.4Coordinates: 35°42′S 323°24′E / 35.7°S 323.4°E / -35.7; 323.4
Diameter 137.5 km
Eponym George Ellery Hale

Hale is a 150 by 125 km (93 by 78 mi) crater at 35.7°S, 323.4°E on Mars, just north of Argyre basin. The crater is in the Argyre quadrangle. It was created by an asteroid roughly 35 km (22 mi) across that impacted at an oblique angle about 3.5 to 3.8 billion years ago. The rim and ejecta are eroded and show smaller impacts, but subsequent deposits have covered up small craters within it.[1] On the southern rim of Hale, parts of the crater wall have moved downslope towards the crater’s centre. The surface shows a network of fluvial channels which may have been caused by running water.[2]

It is named after George Ellery Hale.

The wall of Hale Crater has a large number of gullies. Some are pictured below in an image from HiRISE. Unlike, some other gullies on Mars, these are in light-toned materials. Research published in the journal Icarus has found pits in Hale Crater that are caused by hot ejecta falling on ground containing ice. The pits are formed by heat forming steam that rushes out from groups of pits simultaneously, thereby blowing away from the pit ejecta.[3]


Gullies occur on steep slopes, especially craters. Gullies are believed to be relatively young because they have few, if any craters, and they lie on top of sand dunes which are young. Usually, each gully has an alcove, channel, and apron. Although many ideas have been put forward to explain them, the most popular involve liquid water either coming from an aquifer or left over from old glaciers.[4]

There is evidence for both 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 an aquifer at the usual depths where the gullies begin.[5] 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. This layer would be perched on top of another layer that prevents water from going down (in geological terms it would be called impermeable). The only direction the trapped water can flow is horizontally. The water could then flow out onto the surface when it reaches a break, like a crater wall. Aquifers are quite common on Earth. A good example is "Weeping Rock" in Zion National Park Utah.[6]

On the other hand, much of the surface of Mars is covered by a thick smooth mantle that is thought to be a mixture of ice and dust. 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. Under certain conditions the ice could melt and flow down the slopes to create gullies. Because there are few craters on this mantle, the mantle is relatively young.

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 ice at the top of the mantling layer goes back into the atmosphere, it leaves behind dust, which insulating the remaining ice.[7]

References[edit]

  1. ^ Naeye, Robert (June 2005). "Mars's Hale Crater". Sky and Telescope. 
  2. ^ ESA - Mars Express - Crater Hale in Argyre basin
  3. ^ Tornabene, L. et al. 2012. Widespread crater-related pitted materials on Mars. Further evidence for the role of target volatiles during the impact process. Icarus. 220: 348-368.
  4. ^ Heldmann, J. and M. Mellon. Observations of Martian gullies and constraints on potential formation mechanisms. 2004. Icarus. 168: 285-304.
  5. ^ Heldmann, J. and M. Mellon. 2004. Observations of Martian gullies and constraints on potential formation mechanisms. Icarus. 168:285-304
  6. ^ Harris, A and E. Tuttle. 1990. Geology of National Parks. Kendall/Hunt Publishing Company. Dubuque, Iowa
  7. ^ MLA NASA/Jet Propulsion Laboratory (2003, December 18). Mars May Be Emerging From An Ice Age. ScienceDaily. Retrieved February 19, 2009, from http://www.sciencedaily.com /releases/2003/12/031218075443.htmAds by GoogleAdvertise

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