Phoenicis Lacus quadrangle - Revision history

Suitupshowup at 14:07, 24 January 2025

2025-01-24T14:07:37Z

Suitupshowup at 00:00, 23 January 2025

2025-01-23T00:00:21Z

Suitupshowup: /* Craters */ added more descriptions and ref

2025-01-22T23:59:02Z

Craters: added more descriptions and ref

Suitupshowup: added new info and ref

2024-03-28T15:44:22Z

added new info and ref

Suitupshowup: /* Noctis Labyrinthus */

2023-12-23T22:24:58Z

Noctis Labyrinthus

Suitupshowup: added image

2023-11-25T01:56:40Z

added image

Suitupandshowup: /* External links */

2020-03-27T16:50:27Z

External links

Suitupandshowup at 16:45, 27 March 2020

2020-03-27T16:45:41Z

Suitupandshowup: /* External links */

2020-03-22T16:29:37Z

External links

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2020-03-22T16:19:26Z

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 |[[Mars Atlas|Atlas]]
 |}
 <gallery widths="400" heights="300">
 File:USGS-Mars-MC-17-PhoenicisRegion-mola.png

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 Impact craters are created when a fast moving body strikes the surface.  The force of the impact pushes the ground under the impact point.  Next the ground may rebound thereby thowing material out and around the crater.  Debris lands around the crater forming what is called an ejecta blanket.  This blanket contains samples from deep in the crater.  Sometimes the impact reaches a layer of a different tone then the top layer.  As a consequence, the ejecta may be laid out against a dark background.  these can be quite pretty.  Also, in fresh craters, layers may be exposed on the crater wall; thus, showing past geology.
-When first created a crater is bowl shaped.  With time it becomes more shallow and may develop a flat floor. When yound, layers are visible along the walls of the crater; hence, we can get insight into the geology of the region.  A young crater will still have a bowl shape, a rim, and will show detail in its ejecta.  Relative age of an area is found by examining the density of craters.  Older surfaces will show more craters.
+When first created a crater is bowl shaped.  With time it becomes more shallow and may develop a flat floor. When young, layers are visible along the walls of the crater; hence, we can get insight into the geology of the region.  A young crater will still have a bowl shape, a rim, and will show detail in its ejecta.  Relative age of an area is found by examining the density of craters.  Older surfaces will show more craters.
   <ref>{{cite web | url=https://askanearthspacescientist.asu.edu/top-question/how-craters-form#:~:text=For%20example%2C%20rocks%20collected%20from,energy%20to%20the%20surrounding%20rock | title=How Are Craters Formed? | date=25 June 2019 }}</ref>

← Older revision		Revision as of 23:59, 22 January 2025
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	==Craters==		==Craters==
		+
		+	Impact craters are created when a fast moving body strikes the surface. The force of the impact pushes the ground under the impact point. Next the ground may rebound thereby thowing material out and around the crater. Debris lands around the crater forming what is called an ejecta blanket. This blanket contains samples from deep in the crater. Sometimes the impact reaches a layer of a different tone then the top layer. As a consequence, the ejecta may be laid out against a dark background. these can be quite pretty. Also, in fresh craters, layers may be exposed on the crater wall; thus, showing past geology.
		+	When first created a crater is bowl shaped. With time it becomes more shallow and may develop a flat floor. When yound, layers are visible along the walls of the crater; hence, we can get insight into the geology of the region. A young crater will still have a bowl shape, a rim, and will show detail in its ejecta. Relative age of an area is found by examining the density of craters. Older surfaces will show more craters.
		+	<ref>{{cite web \| url=https://askanearthspacescientist.asu.edu/top-question/how-craters-form#:~:text=For%20example%2C%20rocks%20collected%20from,energy%20to%20the%20surrounding%20rock \| title=How Are Craters Formed? \| date=25 June 2019 }}</ref>

	<gallery class="center" widths="380px" heights="360px">		<gallery class="center" widths="380px" heights="360px">

← Older revision		Revision as of 15:44, 28 March 2024
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	The most common form of volcanism on the Earth is basaltic. Basalts formed from molten rocks that cooled on the surface. They originated from the partial melting of the upper mantle. They are rich in the elements iron and magnesium (so they are classified as mafic minerals) and are commonly dark gray in color. The principal type of volcanism on Mars is probably also basaltic.<ref>Carr \| first1=Michael H. \| publisher=Cambridge University Press \| isbn= 978-0-521-87201-0 \| title= The Surface of Mars \|year=2006 \| ref =harv \| location=New York</ref> Although Mars displays numerous volcanoes here and in other places, there has been no evidence of recent volcanic activity, even at a very low level. Research, from 2017, found no active release of volcanic gases during two successive Martian years. The research team looked for the outgassing of sulfur-bearing chemicals with spectrometers.<ref>Khayat, A., et al. 2017. A deep search for the release of volcanic gases on Mars using ground-based high-resolution infrared and submillimeter spectroscopy: Sensitive upper limits for OCS and SO2. Icarus: 296, 1-14.</ref>		The most common form of volcanism on the Earth is basaltic. Basalts formed from molten rocks that cooled on the surface. They originated from the partial melting of the upper mantle. They are rich in the elements iron and magnesium (so they are classified as mafic minerals) and are commonly dark gray in color. The principal type of volcanism on Mars is probably also basaltic.<ref>Carr \| first1=Michael H. \| publisher=Cambridge University Press \| isbn= 978-0-521-87201-0 \| title= The Surface of Mars \|year=2006 \| ref =harv \| location=New York</ref> Although Mars displays numerous volcanoes here and in other places, there has been no evidence of recent volcanic activity, even at a very low level. Research, from 2017, found no active release of volcanic gases during two successive Martian years. The research team looked for the outgassing of sulfur-bearing chemicals with spectrometers.<ref>Khayat, A., et al. 2017. A deep search for the release of volcanic gases on Mars using ground-based high-resolution infrared and submillimeter spectroscopy: Sensitive upper limits for OCS and SO2. Icarus: 296, 1-14.</ref>
		+
		+	The dsovery of a new volcano at the east side of Noctis Labrinthus was announced at a conference in March 2024. It was seen since the early 1970s, but erosion had concealed it from view.
		+	The new volcano has a diameter of about 280 miles (450 kilometers and measures roughly 29,600 feet (9,022 meters) in elevation. Note: this mountain is higher than any peak in the United States. Lava flows, pyroclastic deposits (made of volcanic materials such as ash, cinders, pumice and tephra) and hydrothermal mineral deposits occur in several areas nearby.<ref>https://www.space.com/mars-giant-volcano-hiding-plain-sight?utm_term=CABA215D-3D47-4C9A-92FE-9ECF8D4C7909&lrh=e62336263a3610a07ef7c8af2080c758f2ecd0661aab1a8e6234cf31f0d0fdff&utm_campaign=58E4DE65-C57F-4CD3-9A5A-609994E2C5A9&utm_medium=email&utm_content=DBDE44BA-0009-4913-99AB-1A1AD0DC4FF9&utm_source=SmartBrief</ref> The volcano is located at 7.40°S, 94.60°W. The authors of the paper consider the volcano to be an eroded shield
		+	volcano. Sub-circular depressions near the top are interpreted as caldera remnants.<ref>https://www.hou.usra.edu/meetings/lpsc2024/pdf/2745.pdf</ref>
		+

	<gallery class="center" widths="380px" heights="360px">		<gallery class="center" widths="380px" heights="360px">

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 [[File: 28370noctis.jpg|600pxr|Layers in a section near the top of wall in Noctis Labyrinthus]]
-                                     Layers in a section near the top of wall in Noctis Labyrinthus
+                   Layers in a section near the top of wall in Noctis Labyrinthus
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 [[File:ESP_027592_1685close.jpg|600pxr|Close-up of layers on floor of Noctis Labyrinthus, as seen by HiRISE [[HiWish program]]]]
-                        Close-up of layers on floor of Noctis Labyrinthus, as seen by HiRISE [[HiWish program]]
+              Close-up of layers on floor of Noctis Labyrinthus, as seen by HiRISE [[HiWish program]]
 == Lava channels ==

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 Image:Arsia mons2.jpg|Arsia Mons, as seen by Mars Global Surveyor.
 Image:Small Volcano mgs.jpg|Small Volcano in Phoenicis Lacus quadrangle. Image is 1.9 miles wide.
+File:Volcano and impact crater 45777 1765.jpg|Volcanic crater (upper) and impact crater (lower)  Image about 5 km across.
 Image:24811lavaflowshill.jpg|Lava flows moving around higher ground, as seen by HiRISE under [[HiWish program]]

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 == External links ==
-*[[https://www.uahirise.org/PSP_005383_1255 Changes in dust devil tracks]]
 *[https://static.uahirise.org/images/2020/details/cut/ESP_063204_1800.gif Looking for Slope Streaks-old and new pictures of streaks]]
 *[https://static.uahirise.org/images/2020/details/cut/ESP_062948_2175.gif New impact fading]

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 [[Category:  Mars Atlas]]
-The Phoenicis Lacus quadrangle contains a mysterious system of interconnected canyons called Noctis Labyrinthus.  In some pictures it looks like a fancy chandelier.  The region is part of the great volcanic area known as Tharsis, Tharsis plateau, Tharsis rise, or Tharsis Bulge.   This quadrangle has a large volcano named Arsia Mons and part of another (Pavonis Mons). Pavonis Mons is good for finding locations, for it sits right on the equator. So, if you are looking at a picture of Mars, you can know for certain where the equator is--just look for the middle volcano of the three that are in a line. The names of some other parts of this quadrangle are Syria Planum, and Claritas Fossae. The classic regions Daedalia Planum, Sinai Planum, and Solis Planum are found in this quadrangle.  Phoenicis Lacus is named after the phoenix which according to myth burns itself up every 500 years and then is reborn.<ref>Blunck, J.  1982.  Mars and its Satellites.  Exposition Press.  Smithtown, N.Y.</ref>
+The Phoenicis Lacus quadrangle contains a mysterious system of interconnected canyons called Noctis Labyrinthus.  In some pictures it looks like a fancy chandelier.  The region is part of the great volcanic area known as Tharsis, Tharsis plateau, Tharsis rise, or Tharsis Bulge.   This quadrangle has a large volcano named Arsia Mons and part of another (Pavonis Mons). Pavonis Mons is good for finding locations, for it sits right on the equator. So, if you are looking at a picture of Mars, you can know for certain where the equator is--just look for the middle volcano of the three that are in a line. The names of some other parts of this quadrangle are Syria Planum, and Claritas Fossae. The classic regions Daedalia Planum, Sinai Planum, and Solis Planum are found in this quadrangle.
 The Phoenicis Lacus quadrangle covers the area from 0° to 30° south latitude and 90° to 135° west longitude (270-225E).
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 The Tharsus rise, which was formed from lava flows, occupies much of the surface. The volcanoes Pavonis Mons and Arsia Mons are believed to have once had glaciers on them. Glaciers may still exist under a thin layer of rocks.<ref>http://www.mars.asu/christensen/advancedmarsclass/shean_glaciers_2005.pdf</ref>  Ice from glaciers can be a source of water for the possible future colonization of the planet.
-Besides some giant volcanoes, there are several other interesting features here including lava channels, Dark slope streaks, pits, and large troughs (called fossae). Pits in Zumba Crater are believed to be caused by hot crater ejecta creating steam after falling on ground containing ice. The pits were formed by steam rushing  out from groups of pits simultaneously, thereby blowing away from the pit ejecta.<ref>Boyce, J. et al. 2012. Origin of small pits in martian impact craters. Icarus. 221: 262-275.</ref> <ref>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.</ref>
+Besides some giant volcanoes, there are several other interesting features here including lava channels, dark slope streaks, pits, and large troughs (called fossae). Pits in Zumba Crater are believed to be caused by hot crater ejecta creating steam after falling on ground containing ice. The pits were formed by steam rushing  out from groups of pits simultaneously, thereby blowing away from the pit ejecta.<ref>Boyce, J. et al. 2012. Origin of small pits in martian impact craters. Icarus. 221: 262-275.</ref> <ref>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.</ref>
 ==Noctis Labyrinthus==
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 Image:Part_of_Noctis_Labyrinthus_taken_with_the_Mars_Global_Surveyor_-_20060529.jpg|Part of Noctis Labyrinthus taken with Mars Global Surveyor. The rectangle indicates where a high resolution picture was taken.  Courtesy NASA/Malin Space Science Systems.
-Image:Noctis_Labyrinthus.JPG|Layers in the wall of Noctis Labyrinthus taken with [[Mars Global Surveyor]],under the MOC Public Targeting Program. This image is within the rectangle in the previous image.Courtesy NASA/Malin Space Science Systems.
 Image:26682layersnorth.jpg|Close-up of some layers in wall of Noctis Labyrinthus
@@ Line 56: / Line 59: @@
 <gallery class="center"  widths="380px" heights="360px">
-ESP 040093 1665layeredmesa.jpg|Layered mesa on floor of Noctis Labyrinthus
+ESP 040093 1665layeredmesa.jpg|Layered mesa on floor of Noctis Labyrinthus  These layers may have formed with water that was at the bottom of Noctis Labyrinthus.
 ESP 040093 1665white.jpg|Enlargement of a light-toned structure on floor of Noctis Labyrinthus
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 == Dark slope streaks ==
-A picture below shows dark slope streaks on Aganippe Fossa. Such streaks are common on Mars. They occur on steep slopes of craters, troughs, and valleys. The streaks are dark at first, and then they get lighter with age. Sometimes they start in a tiny spot, then spread out and go for hundreds of meters. They have been seen to travel around obstacles, like boulders.  It is believed that they are avalanches of bright dust that expose a darker underlying layer. However, several ideas have been advanced to explain them.  The streaks appear in areas covered with dust. Much of the Martian surface is covered with dust. Fine dust settles out of the atmosphere covering everything. We know a lot about this dust because the solar panels of the Mars Rovers got covered with dust, which greatly reduced available  electrical energy. The power of the Rovers was restored many times by the wind, in the form of dust devils, cleaning the panels and boosting the power. So, we know that dust settles from the atmosphere then returns over and over.<ref>https://www.sciencedaily.com/releases/2009/02/090217101110.htm |title=Mars Spirit Rover Gets Energy Boost From Cleaner Solar Panels |publisher=Sciencedaily.com |date=2009-02-19 |</ref> Dust storms are frequent, especially when the spring season begins in the southern hemisphere. At that time, Mars is 40% closer to the sun. The orbit of Mars is much more elliptical then the Earth's. The difference between the farthest point from the sun and the closest point to the sun is very great for Mars, but only a slight amount for the Earth--this fact makes for much more intense seasonal changes.. Also, every few years, the entire planet is engulfed in global dust storms. When NASA's Mariner 9 craft arrived there, nothing could be seen through the dust storm.<ref>Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|accessdate=7 March 2011|date=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7</ref> Other global dust storms have also been observed, since that time.
+A picture below shows dark slope streaks on Aganippe Fossa. Such streaks are common on Mars. They occur on steep slopes of craters, troughs, and valleys. The streaks are dark at first, and then they get lighter with age. Sometimes they start in a tiny spot, then spread out and go for hundreds of meters. They have been seen to travel around obstacles, like boulders.  It is believed that they are avalanches of bright dust that expose a darker underlying layer. However, several ideas have been advanced to explain them.  The streaks appear in areas covered with dust. Much of the Martian surface is covered with dust. Fine dust settles out of the atmosphere covering everything. We know a lot about this dust because the solar panels of the Mars Rovers got covered with dust, which greatly reduced available  electrical energy. The power of the Rovers was restored many times by the wind, in the form of dust devils, cleaning the panels and boosting the power. So, we know that dust settles from the atmosphere then returns over and over.<ref>https://www.sciencedaily.com/releases/2009/02/090217101110.htm |title=Mars Spirit Rover Gets Energy Boost From Cleaner Solar Panels |publisher=Sciencedaily.com |date=2009-02-19 |</ref> Dust storms are frequent, especially when the spring season begins in the southern hemisphere. At that time, Mars is 40% closer to the sun. The orbit of Mars is much more elliptical then the Earth's. The difference between the farthest point from the sun and the closest point to the sun is very great for Mars, but only a slight amount for the Earth--this fact makes for much more intense seasonal changes. Also, every few years, the entire planet is engulfed in global dust storms. When NASA's Mariner 9 craft arrived there, nothing could be seen through the dust storm.<ref>Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|accessdate=7 March 2011|date=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7</ref> Other global dust storms have also been observed, since that time.
 <gallery class="center"  widths="380px" heights="360px">
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 Research that involved streaks close to this quadrangle was published in 2012 in the planetary journal Icarus.  The team found that dark streaks were initiated by airblasts from meteorites traveling at supersonic speeds.    After counting some 65,000 dark streaks around the impact site of a group of 5 new craters, they found some patterns. The number of streaks was greatest closer to the impact site. So, the impact somehow probably caused the streaks.   Also, the distribution of the streaks formed a pattern with two wings extending from the impact site. The curved wings resembled the curved knives, called  scimitars. This pattern suggests that an interaction of airblasts from the group of meteorites shook dust loose enough to start dust avalanches that formed the many dark streaks. At first it was thought that the shaking of the ground from the impact caused the dust avalanches, but if that was the case the dark streaks would have been arranged symmetrically around the impacts, rather than being concentrated into curved shapes.
 The crater cluster lies near the equator 510 miles south of Olympus Mons, on a type of terrain called the Medusae Fossae formation. The formation is coated with dust and contains wind-carved ridges called yardangs. These yardangs have steep slopes thickly covered with dust, so when the sonic boom of the airblast arrived, dust started to move down the slope.
 Using photos from Mars Global Surveyor and HiRISE camera on NASA's Mars Reconnaissance Orbiter, scientists have found about 20 new impacts each year on Mars. Because the spacecraft have been imaging Mars almost continuously for a span of 14 years, newer images with suspected recent craters can be compared to older images to determine when the craters were formed. Since the craters in this study were spotted in a HiRISE image from February 2006, but were not present in a Mars Global Surveyor image taken in May 2004, the impact occurred in that roughly 2-year time frame.
 The largest crater in the cluster is about 22 m in diameter and had an area about like that of a basketball court. As the meteorite traveled through the Martian atmosphere it probably broke up; hence a tight group of craters resulted.
 Dark slope streaks have been seen for some time, and many ideas have been advanced to explain them. This research may have finally solved this mystery.<ref>Kaylan J. Burleigh, Henry J. Melosh, Livio L. Tornabene, Boris Ivanov, Alfred S. McEwen, Ingrid J. Daubar. Impact air blast triggers dust avalanches on Mars. Icarus, 2012; 217 (1): 194 doi|10.1016/j.icarus.2011.10.026</ref> <ref>http://redplanet.asu.edu/</ref>
@@ Line 143: / Line 147: @@
 1580craterlayerssouth.jpg|Close view of layers in crater
 Image:Zumba Crater.JPG|Zumba Crater, as seen by HiRISE. Zumba Crater is a very young crater.
-File:53714 1570craterboulders.jpg|Small crater  Much of the ejecta consists of boulders.
+File:53714 1570craterboulders.jpg|Small crater  Much of its ejecta consists of boulders.
 File:ESP 059649 1695craterpretty.jpg|Young crater with bright ejecta  The impact reached down to a layer that is light-toned.  That light-toned material was then deposited on a dark surface.
 </gallery>
@@ Line 152: / Line 158: @@
-Image:New Impact.JPG|New Impact that formed between March 2000 and July 2003. Scale bar is 500 meters long. Image taken with HiRISE.
 File:ESP 054796 1460channel.jpg|Channel Arrows indicate position of channel in this rather dark photo.
 </gallery>

← Older revision		Revision as of 16:29, 22 March 2020
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	*[[https://www.uahirise.org/PSP_005383_1255 Changes in dust devil tracks]]		*[[https://www.uahirise.org/PSP_005383_1255 Changes in dust devil tracks]]
	*[https://static.uahirise.org/images/2020/details/cut/ESP_063204_1800.gif Looking for Slope Streaks-old and new pictures of streaks]]		*[https://static.uahirise.org/images/2020/details/cut/ESP_063204_1800.gif Looking for Slope Streaks-old and new pictures of streaks]]
		+	*[https://static.uahirise.org/images/2020/details/cut/ESP_062948_2175.gif New impact fading]

← Older revision		Revision as of 16:19, 22 March 2020
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	== External links ==		== External links ==
	*[[https://www.uahirise.org/PSP_005383_1255 Changes in dust devil tracks]]		*[[https://www.uahirise.org/PSP_005383_1255 Changes in dust devil tracks]]
		+	*[https://static.uahirise.org/images/2020/details/cut/ESP_063204_1800.gif Looking for Slope Streaks-old and new pictures of streaks]]