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{{Baustelle}}
{{MarsGeo
|name=Noachis quadrangle
|image=[[File:USGS-Mars-MC-27-NoachisRegion-mola.png|300px]]
|caption=Map of Noachis quadrangle from [[Mars Orbiter Laser Altimeter]] (MOLA) data. The highest elevations are red and the lowest are blue.
|location=
|latitude=47.5
|N_or_S=S
|longitude=330
|E_or_W=W
|type=
|dimensions=
|discoverer=
|naming=
}}
[[File:Noachis Terra.jpg|thumb|300px|Image of the Noachis Quadrangle (MC-27). The northeast includes the western half of [[Hellas basin]]. The southeastern region contains [[Peneus Patera]] and part of the ''Amphitrites volcano''.]]
The '''Noachis 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 Noachis quadrangle is also referred to as MC-27 (Mars Chart-27).<ref>Davies, M.E.; Batson, R.M.; Wu, S.S.C. "Geodesy and Cartography" in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; Matthews, M.S., Eds. ''Mars.'' University of Arizona Press: Tucson, 1992.</ref>


The Noachis quadrangle covers the area from 300° to 360° west longitude and 30° to 65° south latitude on [[Mars]]. It lies between the two giant impact basins on Mars: Argyre and Hellas. The Noachis quadrangle includes [[Noachis Terra]] and the western part of [[Hellas Planitia]].
'''Victor Tobler''', (* [[13. Januar]] [[1846]] in [[Trogen]]; † [[8. Februar]] [[1915]] in [[München]]) war ein Genremaler und Illustrator.


Victor Tobler war alsSohn vom Kaufmann und Ratsherrn Johann Jakob Tobler und Susanna Ernestine Fehr geboren. Im Alter von elf Jahren verlor er seinen Vater und siedelte 1860 mit seiner Mutter nach St. Gallen über.
Noachis is so densely covered with [[impact crater]]s that it is considered among the oldest landforms on Mars—hence the term "[[Noachian]]" for one of the earliest time periods in martian history.
In addition, many previously buried craters are now coming to the surface,<ref>{{cite web|url=http://themis.asu.edu/zoom-20040317a|title=Exhumed Crater (Released 17 March 2004)|author=Mars Space Flight Facility|date=17 March 2004|publisher=Arizona State University|accessdate=19 December 2011}}</ref> where Noachis' extreme age has allowed ancient craters to be filled, and once again newly exposed.


Seinen ersten Malunterricht erhielt er beim Zeichnungslehrer Johann Wilhelm Völker. Danach kam er in das Atelier von [[Rudolf Koller]].
Much of the surface in Noachis quadrangle shows a scalloped topography where the disappearance of ground ice has left depressions.<ref name="Lefort, A. 2010">{{cite journal | last1 = Lefort | first1 = A. | display-authors = 1 | last2 = et al | year = 2010 | title = Scalloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE | url = | journal = Icarus | volume = 205 | issue = | pages = 259–268 | doi=10.1016/j.icarus.2009.06.005 | bibcode=2010Icar..205..259L}}</ref><ref name="sciencedirect.com">http://www.sciencedirect.com/science/journal/00191035</ref>


Tobler begann sein Studium am 20. Mai 1863 an der [[Akademie der Bildenden Künste München]] bei [[Wilhelm Lindenschmit der Jüngere|Wilhelm Lindenschmit dem Jüngeren]]. Seine Vorbilder waren [[Wilhelm von Kaulbach]] und [[Moritz von Schwind]].
The first piece of human technology to land on Mars landed (crashed) in the Noachis quadrangle. The Soviet's [[Mars 2]] crashed at {{Coord|44.2|S|313.2|W|globe:Mars}}. It weighed about one ton. The automated craft attempted to land in a giant dust storm. To make conditions even worse, this area also has many dust devils.<ref>Hartmann, W. 2003. A Traveler's Guide to Mars. Workman Publishing. NY, NY.</ref>


Im Militardienst wurde er zum Offizier der Artillerie befördert.
==Scalloped topography==
[[Image:Scalloped Terrain at Peneus Patera.JPG|thumb|Scalloped Terrain at [[Peneus Patera]], as seen by HiRISE. Scalloped terrain is quite common in some areas of Mars.]]
Certain regions of Mars display [[scalloped topography|scalloped-shaped depressions]]. The depressions are believed to be the remains of an ice-rich mantle deposit. Scallops are created when ice sublimates from frozen soil. This mantle material probably fell from the air as ice formed on dust when the climate was different due to changes in the tilt of the Mars pole.<ref>Head, J. et al. 2003. Recent ice ages on Mars. Nature:426. 797-802.</ref> The scallops are typically tens of meters deep and from a few hundred to a few thousand meters across. They can be almost circular or elongated. Some appear to have coalesced, thereby causing a large heavily pitted terrain to form. A study published in Icarus, found that the landforms of scalloped topography can be made by the subsurface loss of water ice by sublimation under current Martian climate conditions. Their model predicts similar shapes when the ground has large amounts of pure ice, up to many tens of meters in depth.<ref>Dundas, C., S. Bryrne, A. McEwen. 2015. Modeling the development of martian sublimation thermokarst landforms. Icarus: 262, 154-169.</ref>
The process of producing the terrain may begin with sublimation from a crack because there are often polygon cracks where scallops form.<ref name="Lefort, A. 2010"/><ref name="sciencedirect.com"/>


Victor Tobler blieb in München und wurde zum Vorstand der Munchner Künstlergenossenschaft gewählt.
== Dust Devil Tracks ==
Many areas on Mars experience the passage of giant [[dust devils]]. A thin coating of fine bright dust covers most of the Martian surface. When a dust devil goes by it blows away the coating and exposes the underlying dark surface creating [[Dust Devil Tracks|tracks]]. Dust devils have been seen from the ground and from orbit. They have even blown the dust off of the [[solar panels]] of the two [[Mars Exploration Rover|Rovers on Mars]], thereby greatly extending their lives.<ref>{{cite web|url=http://marsrovers.jpl.nasa.gov/gallery/press/spirit/20070412a.html|title=Press Release Images: Spirit|date=12 April 2007|publisher=[[National Aeronautics and Space Administration]]|accessdate=19 December 2011}}</ref> The twin Rovers were designed to last for 3 months, instead they have lasted more than six years and are still going after over 8 years. The pattern of the tracks have been shown to change every few months.<ref>{{cite web|url=http://mars.jpl.nasa.gov/spotlight/KenEdgett.html|title=Ken Edgett|date=2001|publisher=National Aeronautics and Space Administration|accessdate=19 December 2011}}</ref> TA study that combined data from the [[High Resolution Stereo Camera]] (HRSC) and the [[Mars Orbiter Camera]] (MOC) found that some large dust devils on Mars have a diameter of 700 meters and last at least 26 minutes.<ref>{{cite journal | last1 = Reiss | first1 = D. | display-authors = 1 | last2 = et al | year = 2011 | title = Multitemporal observations of identical active dust devils on Mars with High Resolution Stereo Camera (HRSC) and Mars Orbiter Camera (MOC) | url = | journal = Icarus | volume = 215 | issue = | pages = 358–369 | doi=10.1016/j.icarus.2011.06.011 | bibcode=2011Icar..215..358R}}</ref> The image below of Russel Crater shows changes in dust devil tracks over a period of only three months, as documented by [[HiRISE]]. Other Dust Devil Tracks are visible in the picture of Frento Vallis.


Jeden Sommer verbrachte er einige Monate im Appenzellerland, wo er sich mit dem dortigen Folklore und der Landschaft beschaftigte.
<gallery>
Image:Russel Crater Dust Devil Changes.JPG|[[Russell (Martian crater)|Russell Crater]] Dust Devil Changes, as seen by [[HiRISE]]. Click on image to see changes in dust devil tracks in just 3 months.
Image:Frento Vallis.JPG|[[Frento Vallis]], as seen by HiRISE. Click on image to see better view of [[Dust Devil Tracks]].
</gallery>


Für seine Söhne Georg und Justus hat Victor Tobler Ende des 19.Jahrhunderts ihr eigenes Marionettentheater gebaut.
==Craters==
Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10&nbsp;km in diameter) they usually have a central peak.<ref name="lpi.usra.edu">http://www.lpi.usra.edu/publications/slidesets/stones/</ref> The peak is caused by a rebound of the crater floor following the impact.<ref name="Kieffer1992">{{cite book|author=Hugh H. Kieffer|title=Mars|url=http://books.google.com/books?id=NoDvAAAAMAAJ|accessdate=7 March 2011|date=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7}}</ref> Sometimes craters will display layers. Craters can show us what lies deep under the surface.


==Why are Craters important?==
The density of impact craters is used to determine the surface ages of Mars and other solar system bodies.<ref name="lpi.usra.edu"/> The older the surface, the more craters present. Crater shapes can reveal the presence of ground ice.


Der Schatz dieser Bühne liegt in der technischen Raffinesse. Es sind Bühnenkonstruktionen zu finden, wie Versenkungen und elektrisches Licht, die es damals an manch grossem Haus nicht gegeben hat. Die Genauigkeit, der grosse Aufwand, die Zartheit und die Detailfreude, mit der an dieser Bühne gearbeitet wurde, zeugen von der Liebe und Faszination für diese Kunstform. Die Bedeutung dieses Marionettentheaters und der ästhetische Anspruch für sich selbst und den Zuschauer, können noch heute entdeckt werden und begeistern, auch wenn die Bühne seit über 100 Jahren unbespielt ist.
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.<ref>http://www.indiana.edu/~sierra/papers/2003/Patterson.html.</ref>
Studies on the earth have documented that cracks are produced and that secondary minerals veins are deposited in the cracks.<ref>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</ref><ref>http://www.ingentaconnect.com/content/arizona/maps/2005/00000040/00000012/art00007</ref><ref>Pirajno, F. 2000. Ore Deposits and Mantle Plumes. Kluwer Academic Publishers. Dordrecht, The Netherlands</ref> Images from satellites orbiting Mars have detected cracks near impact craters.<ref>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</ref> Great amounts of heat are produced during impacts. The area around a large impact may take hundreds of thousands of years to cool.<ref>name="news.discovery.com"</ref><ref>Segura, T, O. Toon, A. Colaprete, K. Zahnle. 2001. Effects of Large Impacts on Mars: Implications for River Formation. American Astronomical Society, DPS meeting#33, #19.08</ref><ref>Segura, T, O. Toon, A. Colaprete, K. Zahnle. 2002. Environmental Effects of Large Impacts on Mars. Science: 298, 1977-1980.</ref>
Many craters once contained lakes.<ref>Cabrol, N. and E. Grin. 2001. The Evolution of Lacustrine Environments on Mars: Is Mars Only Hydrologically Dormant? Icarus: 149, 291-328.</ref><ref>Fassett, C. and J. Head. 2008. Open-basin lakes on Mars: Distribution and implications for Noachian surface and subsurface hydrology. Icarus: 198, 37-56.</ref><ref>Fassett, C. and J. Head. 2008. Open-basin lakes on Mars: Implications of valley network lakes for the nature of Noachian hydrology.</ref> 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.<ref>Wilson, J. A. Grant and A. Howard. 2013. INVENTORY OF EQUATORIAL ALLUVIAL FANS AND DELTAS ON MARS. 44th Lunar and Planetary Science Conference.</ref> 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.<ref>Newsom H. , Hagerty J., Thorsos I. 2001. Location and sampling of aqueous and hydrothermal deposits in martian impact craters. Astrobiology: 1, 71-88.</ref>


<gallery>
Image:Maunder Crater.JPG|[[Maunder Crater]], as seen by HiRISE. The overhang is part of the degraded south (toward bottom) wall of crater. The scale bar is 500 meters long.
Image:Asimov Crater.jpg|[[Asimov Crater]], as seen by HiRISE. Bottom of picture shows southeastern wall of crater. Top of picture is edge of mound that fills most of the crater.
Image:Asimov Crater Layers.jpg|Layers in west slope of Asimov Crater, as seen by HiRISE.
Image:Asimov Layers Close-up.JPG|Close-up of layers in west slope of Asimov Crater. Shadows show the overhang. Some of the layers are much more resistant to erosion, so they stick out. Image from HiRISE.
Image:Asimov Crater Central Pit.jpg|East Slope of Central Pit in Asimov Crater, as seen by HiRISE. Click on image to see more details of the many gullies.
Image:Kaiser Crater.JPG|[[Kaiser Crater]] (large crater in upper part of image)context for [[THEMIS]] image.
Image:Kaiser Crater.jpg|Detail of south wall of Kaiser Crater, as seen by THEMIS. Top of image shows part of a dune field.
Image:Rabe Crater Floor.JPG|[[Rabe Crater]] Floor, as seen by [[HiRISE]]. Click on image to see layers. Dark sand that made the dunes was probably blown in from elsewhere.
Image:Exhumed crater in Noachis.JPG|Crater that was buried in another age and is now being exposed by erosion, as seen by the [[Mars Global Surveyor]], under the [[MOC Public Targeting Program]].
Image:24396floor.jpg|Floor of crater in Noachis quadrangle, as seen by HiRISE under [[HiWish program]].
ESP 035632 1490noachiscraterfloor.jpg|Erosion forms on floor of crater, as seen by HiRISE under HiWish program
</gallery>


==Sand Dunes==
When there are perfect conditions for producing sand dunes, steady wind in one direction and just enough sand, a barchan sand dune forms. Barchans have a gentle slope on the wind side and a much steeper slope on the lee side where horns or a notch often forms.<ref name=Pye2008>{{cite book|last=Pye|first=Kenneth|title=Aeolian Sand and Sand Dunes|year=2008|publisher=Springer|isbn=9783540859109|pages=138|author2=Haim Tsoar}}</ref> One picture below shows a definite barchan.
<gallery>
Image:Dark dunes in Noachis.JPG|Dark dunes (probably [[basalt]]), in an intracrater dune field, Noachis. Picture from Mars Global Surveyor, under the [[MOC Public Targeting Program]].
Image:Dunes Wide View.jpg|Wide view of dunes in Noachis, as seen by HiRISE.
Image:Close-up view of Dunes.jpg|Close-up View of dunes in previous image, as seen by HiRISE. Note how sand barely covers some boulders.
Image:Barchan in Noachis.jpg|[[Barchan]] sand dunes in the Hellespontus region, as seen by HiRISE. The horns point in the downwind direction.
Image:Proctor Crater Ripples and Dunes.JPG|[[Proctor Crater]] ripples and dunes, as seen by HiRISE.
</gallery>


== Gallery ==
== Literatur ==
* [http://www.sikart.ch/kuenstlerinnen.aspx?id=4023306&lng=de Sikart]
<gallery>
* [https://www.google.pl/?gws_rd=ssl#q=Victor+Tobler Hermann Grosser: Victor Tobler, ein Appenzeller Maler der Jahrhundertwende Appenzeller Kalender 1972]
Image:Noachis Map.JPG|Quadrangle map of Noachis labeled with major features.
* [https://www.google.pl/?gws_rd=ssl#q=Victor+Tobler H. Pfenninger Victor Tobler ein Appenzellischer Maler Heimatschutz Heft 2/1917]
Image:Dissected Mantle.JPG|Dissected Mantle with layers, as seen by HiRISE.
* [https://www.amazon.de/Toblers-Marionettentheater-von-1897-1900-Marionettenb%C3%BChne/dp/3639300858 Danielle Strahm: Toblers Marionettentheater von 1897-1900]
Image:Twisted Terrain in Hellas Planitia.jpg|Twisted Terrain in [[Hellas Planitia]], but actually located in Noachis quadrangle. Imagine trying to walk across this. Image taken with HiRISE.
*{{Commonscat}}

{{Normdaten|TYP=p|GND=|VIAF=}}
Esp 037147 1430layers.jpg|Layers in depression in crater, as seen by HiRISE under HiWish program
{{SORTIERUNG:}}<!--

[[Kategorie:Maler (Deutschland)]]
</gallery>
[[Kategorie:Geboren 18]]

[[Kategorie:Gestorben 19]]
==Gullies==
[[Kategorie:Mann]]
Gullies on steep slopes are found in certain regions of Mars. Many ideas have been advanced to explain them. Formation by running water when the climate was different is a popular idea. Recently, because changes in gullies have been seen since HiRISE has been orbiting Mars, it is thought that they may be formed by chunks of dry ice moving down slope during spring time. Gullies are one of the most interesting discoveries made by orbiting space craft.<ref>http://www.jpl.nasa.gov/news/news.php?release=2014-226</ref><ref>http://hirise.lpl.arizona.edu/ESP_032078_1420</ref><ref>http://www.space.com/26534-mars-gullies-dry-ice.html?cmpid=557882</ref><ref>http://spaceref.com/mars/frosty-gullies-on-mars.html</ref>
{{Personendaten
<gallery>
|NAME=
ESP 037793 1445noachisgullies.jpg|Gullies on the wall of a crater, as seen by HiRISE under HiWish program
|ALTERNATIVNAMEN=
Image:Close-up of Asimov Crater.JPG|Gullies on mound in Asimov Crater, as seen by HiRISE.
|KURZBESCHREIBUNG=deutscher Maler und Grafiker
</gallery>
|GEBURTSDATUM=

|GEBURTSORT=[[]]
==See also==
|STERBEDATUM=1938
* [[Climate of Mars]]
|STERBEORT=[[]]
* [[Geology of Mars]]
}}
* [[List of quadrangles on Mars]]
-->
* [[Water on Mars]]
* [[Martian gullies]]
* [[Planetary nomenclature]]
* [[Impact crater]]
* [[List of craters on Mars]]
* [[Ore genesis]]
* [[Ore resources on Mars]]
* [[Hydrothermal circulation]]
* [[Barchan]]
* [[Groundwater on Mars]]

==References==
{{reflist|30em}}

{{commons category|Noachis quadrangle}}
{{Mars Quads - By Name}}
{{Mars quadrangle layout}}
{{Mars}}

{{portal bar|Mars}}

{{DEFAULTSORT:Noachis Quadrangle}}
[[Category:Noachis quadrangle| ]]

Version vom 16. September 2016, 09:39 Uhr


Victor Tobler, (* 13. Januar 1846 in Trogen; † 8. Februar 1915 in München) war ein Genremaler und Illustrator.

Victor Tobler war alsSohn vom Kaufmann und Ratsherrn Johann Jakob Tobler und Susanna Ernestine Fehr geboren. Im Alter von elf Jahren verlor er seinen Vater und siedelte 1860 mit seiner Mutter nach St. Gallen über.

Seinen ersten Malunterricht erhielt er beim Zeichnungslehrer Johann Wilhelm Völker. Danach kam er in das Atelier von Rudolf Koller.

Tobler begann sein Studium am 20. Mai 1863 an der Akademie der Bildenden Künste München bei Wilhelm Lindenschmit dem Jüngeren. Seine Vorbilder waren Wilhelm von Kaulbach und Moritz von Schwind.

Im Militardienst wurde er zum Offizier der Artillerie befördert.

Victor Tobler blieb in München und wurde zum Vorstand der Munchner Künstlergenossenschaft gewählt.

Jeden Sommer verbrachte er einige Monate im Appenzellerland, wo er sich mit dem dortigen Folklore und der Landschaft beschaftigte.

Für seine Söhne Georg und Justus hat Victor Tobler Ende des 19.Jahrhunderts ihr eigenes Marionettentheater gebaut.


Der Schatz dieser Bühne liegt in der technischen Raffinesse. Es sind Bühnenkonstruktionen zu finden, wie Versenkungen und elektrisches Licht, die es damals an manch grossem Haus nicht gegeben hat. Die Genauigkeit, der grosse Aufwand, die Zartheit und die Detailfreude, mit der an dieser Bühne gearbeitet wurde, zeugen von der Liebe und Faszination für diese Kunstform. Die Bedeutung dieses Marionettentheaters und der ästhetische Anspruch für sich selbst und den Zuschauer, können noch heute entdeckt werden und begeistern, auch wenn die Bühne seit über 100 Jahren unbespielt ist.


Literatur

Normdaten (Person): Wikipedia-Personensuche
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