Noachis quadrangle - Revision history

Suitupshowup: /* Hellas floor features */ added image

2025-12-05T18:25:28Z

Hellas floor features: added image

Suitupshowup: added image

2025-01-01T14:28:47Z

added image

Suitupshowup: /* Craters */ added image

2024-02-20T15:57:13Z

Craters: added image

Suitupshowup: /* Hellas floor features */

2023-12-23T23:02:34Z

Hellas floor features

Suitupshowup: /* Sand Dunes */

2023-12-23T23:00:49Z

Sand Dunes

Suitupshowup: /* Hellas floor features */ added image

2023-11-18T23:05:43Z

Hellas floor features: added image

Suitupandshowup: /* Hellas floor features */

2023-03-21T00:56:05Z

Hellas floor features

Suitupandshowup: /* Hellas floor features */ added

2023-03-21T00:54:58Z

Hellas floor features: added

Suitupandshowup: /* Hellas floor features */ added new info and ref

2022-02-12T22:54:37Z

Hellas floor features: added new info and ref

Suitupandshowup: /* External links */

2020-03-27T19:08:12Z

External links

← Older revision		Revision as of 18:25, 5 December 2025
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	Banded terrain, as seen by HiRISE under HiWish program		Banded terrain, as seen by HiRISE under HiWish program
		+
		+
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		+	[[File:90251 1380hellascropped.jpg\|600pxr\|Twisted bands on Hellas floor]]
		+
		+	Twisted bands on Hellas floor

	==Gullies on Dunes==		==Gullies on Dunes==

@@ Line 9: / Line 9: @@
 |[[Mars Atlas|Atlas]]
 |}
 <gallery widths="400" heights="300">
 File:USGS-Mars-MC-27-NoachisRegion-mola.png

← Older revision		Revision as of 15:57, 20 February 2024
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	Image:24396floor.jpg\|Floor of crater in Noachis quadrangle, as seen by HiRISE under [[HiWish program]].		Image:24396floor.jpg\|Floor of crater in Noachis quadrangle, as seen by HiRISE under [[HiWish program]].

		+	File:Secondary craters ESP 081458 1425.jpg\|Secondry craters, as seen by HiRISE under HiWish program These were made from material thrown in the air by primary impact of large body nearby.
	</gallery>		</gallery>

@@ Line 143: / Line 143: @@
 [[File:ESP 055067 1420ridgenetwork.jpg|600pxr|Floor features in Hellas Planitia]]
-                                            Floor features in Hellas Planitia
+                             Floor features in Hellas Planitia
@@ Line 152: / Line 152: @@
 [[File:Banded terrain in Hellas Planitia, as seen by HiRISE under HiWish program.jpg|Banded terrain, as seen by HiRISE under HiWish program|600pxr|Banded terrain in Hellas Planitia, as seen by HiRISE under HiWish program.jpg|Banded terrain, as seen by HiRISE under HiWish program]]
-                                 Banded terrain, as seen by HiRISE under HiWish program
+                             Banded terrain, as seen by HiRISE under HiWish program
 ==Gullies on Dunes==

@@ Line 68: / Line 68: @@
 [[File: Dark dunes in Noachis.JPG|600pxr|Wide view of a field of sand dunes]]
-     Wide view of a field of sand dunes, as seen by Mars Global Surveyor
+Wide view of a field of sand dunes, as seen by Mars Global Surveyor
 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>Pye|first=Kenneth|title=Aeolian Sand and Sand Dunes|year=2008|publisher=Springer|isbn=9783540859109|pages=138|</ref>  One picture below shows a definite barchan.
 [[File:ESP 046378 1415dunes.jpg|600pxr|Dark dunes]]
- Wide view of a field of sand dunes
+                            Wide view of a field of sand dunes
 <gallery class="center"  widths="380px" heights="360px">

← Older revision		Revision as of 23:05, 18 November 2023
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	Wide view of twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program		Wide view of twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program
		+
		+	[[File:Banded terrain in Hellas Planitia, as seen by HiRISE under HiWish program.jpg\|Banded terrain, as seen by HiRISE under HiWish program\|600pxr\|Banded terrain in Hellas Planitia, as seen by HiRISE under HiWish program.jpg\|Banded terrain, as seen by HiRISE under HiWish program]]
		+
		+	Banded terrain, as seen by HiRISE under HiWish program

	==Gullies on Dunes==		==Gullies on Dunes==

@@ Line 120: / Line 120: @@
 The Hellas floor contains some strange-looking features.  One of these features is called "banded terrain."<ref>Diot, X., et al.  2014.  The geomorphology and morphometry of the banded terrain in Hellas basin, Mars.  Planetary and Space Science: 101, 118-134.</ref> <ref>http://www.nasa.gov/mission_pages/MRO/multimedia/20070717-2.html | title=NASA - Banded Terrain in Hellas</ref> <ref>http://hirise.lpl.arizona.edu/ESP_016154_1420 | title=HiRISE &#124; Complex Banded Terrain in Hellas Planitia (ESP_016154_1420)</ref>  This terrain has also been called "taffy pull" terrain, and it lies near honeycomb terrain, another strange surface.<ref>Bernhardt, H., et al.  2018.  THE BANDED TERRAIN ON THE HELLAS BASIN FLOOR, MARS: GRAVITY-DRIVEN FLOW NOT SUPPORTED BY NEW OBSERVATIONS.  49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083).  1143.pdf</ref>  Banded terrain is found in the north-western part of the Hellas basin.  This is the deepest part of the Hellas basin.  The banded-terrain deposit displays an alternation of narrow band shapes and inter-bands.  The sinuous nature and relatively smooth surface texture suggesting a viscous flow origin.  A study published in Planetary and Space Science found that this terrain was the youngest deposit of the interior of Hellas.  They also suggest in the paper that banded terrain may have covered a larger area of the NW interior of Hellas.  The bands can be classified as linear, concentric, or lobate.  Bands are typically 3–15 km long, 3 km wide.  Narrow inter-band depressions are 65 m wide and 10 m deep.<ref>Complex geomorphologic assemblage of terrains in association with the banded terrain in Hellas basin, Mars |journal=Planetary and Space Science |volume=121 |pages=36–52 |year=2016 |last1=Diot |first1=X. |last2=El-Maarry |first2=M.R. |last3=Schlunegger |first3=F. |last4=Norton |first4=K.P. |last5=Thomas |first5=N. |last6=Grindrod |first6=P.M. |last7=Chojnacki |first7=M. |bibcode=2016P&SS..121...36D |url=https://boris.unibe.ch/74530/1/Diot_Schlunegger.pdf </ref>  Researchers do not at this time understand how these features ere formed. .<ref>https://www.hou.usra.edu/meetings/lpsc2022/pdf/1588.pdf</ref> <ref>Cook, C., et al.  2022.   FORMATION OF THE BANDED TERRAIN OF HELLAS PLANITIA, MARS. 53rd Lunar and Planetary Science Conference (2022).  1588.pdf</ref>
-One idea for how these strange features were created involves a large mass of ice being deposited into the Hellas basin.  Later the ice could be covered with lava and ash from the many nearby volcanoes.  Hot lava would melt some of the ice, but the heat may not have been enough to melt all the ice.  So, there may have been a thick layer of lava and ash sitting on top of ice.  The ice is much less dense; consequently, it would rise through the denser material that covers it.  Strange shapes could result.  This principle is like when one pulls a ball down int a swimming pool.  The ball would want to go up through the water.  On Earth this type of even occurs.  The bodies that form are called diapirs.  Sometimes salt deposits covered by sediment move upward on the Earth. Diapir comes from Greek diapeirein, which means “to pierce" in reference to how one lower density body pierces or moves through another.<ref> Fastook1, J.  and J.   Head.  2023.   HELLAS BASIN, MARS: RIM-WALL-FLOOR GLACIATION IN THE LATE NOACHIAN-EARLY HESPERIAN AND INTERACTIONS WITH SUPERPOSED LAVA FLOWS.  54th Lunar and Planetary Science Conference 2023 (LPI Contrib. No. 2806).  1330.pdf</ref>
+One idea for how these strange features were created involves a large mass of ice being deposited into the Hellas basin.  Later the ice could be covered with lava and ash from the many nearby volcanoes.  Hot lava would melt some of the ice, but the heat may not have been enough to melt all the ice.  So, there may have been a thick layer of lava and ash sitting on top of ice.  The ice is much less dense; consequently, it would rise through the denser material that covers it.  Strange shapes could result.  This principle is like when one pulls a ball down into a swimming pool.  The ball would want to go up through the water.  On Earth this type of event occurs.  The bodies that form are called diapirs.  Sometimes salt deposits covered by sediment move upward on the Earth. Diapir comes from Greek diapeirein, which means “to pierce" in reference to how one lower density body pierces or moves through another.<ref> Fastook1, J.  and J.   Head.  2023.   HELLAS BASIN, MARS: RIM-WALL-FLOOR GLACIATION IN THE LATE NOACHIAN-EARLY HESPERIAN AND INTERACTIONS WITH SUPERPOSED LAVA FLOWS.  54th Lunar and Planetary Science Conference 2023 (LPI Contrib. No. 2806).  1330.pdf</ref>
 Pictures of these features can look like abstract art.

@@ Line 118: / Line 118: @@
               Close-up of banded terrain on the floor of the Hellas basin, as seen by HiRISE
-The Hellas floor contains some strange-looking features.  One of these features is called "banded terrain."<ref>Diot, X., et al.  2014.  The geomorphology and morphometry of the banded terrain in Hellas basin, Mars.  Planetary and Space Science: 101, 118-134.</ref> <ref>http://www.nasa.gov/mission_pages/MRO/multimedia/20070717-2.html | title=NASA - Banded Terrain in Hellas</ref> <ref>http://hirise.lpl.arizona.edu/ESP_016154_1420 | title=HiRISE &#124; Complex Banded Terrain in Hellas Planitia (ESP_016154_1420)</ref>  This terrain has also been called "taffy pull" terrain, and it lies near honeycomb terrain, another strange surface.<ref>Bernhardt, H., et al.  2018.  THE BANDED TERRAIN ON THE HELLAS BASIN FLOOR, MARS: GRAVITY-DRIVEN FLOW NOT SUPPORTED BY NEW OBSERVATIONS.  49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083).  1143.pdf</ref>  Banded terrain is found in the north-western part of the Hellas basin.  This is the deepest part of the Hellas basin.  The banded-terrain deposit displays an alternation of narrow band shapes and inter-bands.  The sinuous nature and relatively smooth surface texture suggesting a viscous flow origin.  A study published in Planetary and Space Science found that this terrain was the youngest deposit of the interior of Hellas.  They also suggest in the paper that banded terrain may have covered a larger area of the NW interior of Hellas.  The bands can be classified as linear, concentric, or lobate.  Bands are typically 3–15 km long, 3 km wide.  Narrow inter-band depressions are 65 m wide and 10 m deep.<ref>Complex geomorphologic assemblage of terrains in association with the banded terrain in Hellas basin, Mars |journal=Planetary and Space Science |volume=121 |pages=36–52 |year=2016 |last1=Diot |first1=X. |last2=El-Maarry |first2=M.R. |last3=Schlunegger |first3=F. |last4=Norton |first4=K.P. |last5=Thomas |first5=N. |last6=Grindrod |first6=P.M. |last7=Chojnacki |first7=M. |bibcode=2016P&SS..121...36D |url=https://boris.unibe.ch/74530/1/Diot_Schlunegger.pdf </ref>  Researchers do not at this time understand how these features ere formed. .<ref>https://www.hou.usra.edu/meetings/lpsc2022/pdf/1588.pdf</ref> <ref>Cook, C., et al.  2022.   FORMATION OF THE BANDED TERRAIN OF HELLAS PLANITIA, MARS. 53rd Lunar and Planetary Science Conference (2022).  1588.pdf</ref>  Pictures of these features can look like abstract art.
+The Hellas floor contains some strange-looking features.  One of these features is called "banded terrain."<ref>Diot, X., et al.  2014.  The geomorphology and morphometry of the banded terrain in Hellas basin, Mars.  Planetary and Space Science: 101, 118-134.</ref> <ref>http://www.nasa.gov/mission_pages/MRO/multimedia/20070717-2.html | title=NASA - Banded Terrain in Hellas</ref> <ref>http://hirise.lpl.arizona.edu/ESP_016154_1420 | title=HiRISE &#124; Complex Banded Terrain in Hellas Planitia (ESP_016154_1420)</ref>  This terrain has also been called "taffy pull" terrain, and it lies near honeycomb terrain, another strange surface.<ref>Bernhardt, H., et al.  2018.  THE BANDED TERRAIN ON THE HELLAS BASIN FLOOR, MARS: GRAVITY-DRIVEN FLOW NOT SUPPORTED BY NEW OBSERVATIONS.  49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083).  1143.pdf</ref>  Banded terrain is found in the north-western part of the Hellas basin.  This is the deepest part of the Hellas basin.  The banded-terrain deposit displays an alternation of narrow band shapes and inter-bands.  The sinuous nature and relatively smooth surface texture suggesting a viscous flow origin.  A study published in Planetary and Space Science found that this terrain was the youngest deposit of the interior of Hellas.  They also suggest in the paper that banded terrain may have covered a larger area of the NW interior of Hellas.  The bands can be classified as linear, concentric, or lobate.  Bands are typically 3–15 km long, 3 km wide.  Narrow inter-band depressions are 65 m wide and 10 m deep.<ref>Complex geomorphologic assemblage of terrains in association with the banded terrain in Hellas basin, Mars |journal=Planetary and Space Science |volume=121 |pages=36–52 |year=2016 |last1=Diot |first1=X. |last2=El-Maarry |first2=M.R. |last3=Schlunegger |first3=F. |last4=Norton |first4=K.P. |last5=Thomas |first5=N. |last6=Grindrod |first6=P.M. |last7=Chojnacki |first7=M. |bibcode=2016P&SS..121...36D |url=https://boris.unibe.ch/74530/1/Diot_Schlunegger.pdf </ref>  Researchers do not at this time understand how these features ere formed. .<ref>https://www.hou.usra.edu/meetings/lpsc2022/pdf/1588.pdf</ref> <ref>Cook, C., et al.  2022.   FORMATION OF THE BANDED TERRAIN OF HELLAS PLANITIA, MARS. 53rd Lunar and Planetary Science Conference (2022).  1588.pdf</ref>
 [[File:Twisted Terrain in Hellas Planitia.jpg|600pxr|Twisted Terrain in Hellas Planitia, but actually located in Noachis quadrangle.  Imagine trying to walk across this.  Image taken with HiRISE.]]

← Older revision		Revision as of 22:54, 12 February 2022
Line 118:		Line 118:
	Close-up of banded terrain on the floor of the Hellas basin, as seen by HiRISE		Close-up of banded terrain on the floor of the Hellas basin, as seen by HiRISE

−	The Hellas floor contains some strange-looking features. One of these features is called "banded terrain."<ref>Diot, X., et al. 2014. The geomorphology and morphometry of the banded terrain in Hellas basin, Mars. Planetary and Space Science: 101, 118-134.</ref> <ref>http://www.nasa.gov/mission_pages/MRO/multimedia/20070717-2.html \| title=NASA - Banded Terrain in Hellas</ref> <ref>http://hirise.lpl.arizona.edu/ESP_016154_1420 \| title=HiRISE \| Complex Banded Terrain in Hellas Planitia (ESP_016154_1420)</ref> This terrain has also been called "taffy pull" terrain, and it lies near honeycomb terrain, another strange surface.<ref>Bernhardt, H., et al. 2018. THE BANDED TERRAIN ON THE HELLAS BASIN FLOOR, MARS: GRAVITY-DRIVEN FLOW NOT SUPPORTED BY NEW OBSERVATIONS. 49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083). 1143.pdf</ref> Banded terrain is found in the north-western part of the Hellas basin. This is the deepest part of the Hellas basin. The banded-terrain deposit displays an alternation of narrow band shapes and inter-bands. The sinuous nature and relatively smooth surface texture suggesting a viscous flow origin. A study published in Planetary and Space Science found that this terrain was the youngest deposit of the interior of Hellas. They also suggest in the paper that banded terrain may have covered a larger area of the NW interior of Hellas. The bands can be classified as linear, concentric, or lobate. Bands are typically 3–15 km long, 3 km wide. Narrow inter-band depressions are 65 m wide and 10 m deep.<ref>Complex geomorphologic assemblage of terrains in association with the banded terrain in Hellas basin, Mars \|journal=Planetary and Space Science \|volume=121 \|pages=36–52 \|year=2016 \|last1=Diot \|first1=X. \|last2=El-Maarry \|first2=M.R. \|last3=Schlunegger \|first3=F. \|last4=Norton \|first4=K.P. \|last5=Thomas \|first5=N. \|last6=Grindrod \|first6=P.M. \|last7=Chojnacki \|first7=M. \|bibcode=2016P&SS..121...36D \|url=https://boris.unibe.ch/74530/1/Diot_Schlunegger.pdf </ref> Pictures of these features can look like abstract art.	+	The Hellas floor contains some strange-looking features. One of these features is called "banded terrain."<ref>Diot, X., et al. 2014. The geomorphology and morphometry of the banded terrain in Hellas basin, Mars. Planetary and Space Science: 101, 118-134.</ref> <ref>http://www.nasa.gov/mission_pages/MRO/multimedia/20070717-2.html \| title=NASA - Banded Terrain in Hellas</ref> <ref>http://hirise.lpl.arizona.edu/ESP_016154_1420 \| title=HiRISE \| Complex Banded Terrain in Hellas Planitia (ESP_016154_1420)</ref> This terrain has also been called "taffy pull" terrain, and it lies near honeycomb terrain, another strange surface.<ref>Bernhardt, H., et al. 2018. THE BANDED TERRAIN ON THE HELLAS BASIN FLOOR, MARS: GRAVITY-DRIVEN FLOW NOT SUPPORTED BY NEW OBSERVATIONS. 49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083). 1143.pdf</ref> Banded terrain is found in the north-western part of the Hellas basin. This is the deepest part of the Hellas basin. The banded-terrain deposit displays an alternation of narrow band shapes and inter-bands. The sinuous nature and relatively smooth surface texture suggesting a viscous flow origin. A study published in Planetary and Space Science found that this terrain was the youngest deposit of the interior of Hellas. They also suggest in the paper that banded terrain may have covered a larger area of the NW interior of Hellas. The bands can be classified as linear, concentric, or lobate. Bands are typically 3–15 km long, 3 km wide. Narrow inter-band depressions are 65 m wide and 10 m deep.<ref>Complex geomorphologic assemblage of terrains in association with the banded terrain in Hellas basin, Mars \|journal=Planetary and Space Science \|volume=121 \|pages=36–52 \|year=2016 \|last1=Diot \|first1=X. \|last2=El-Maarry \|first2=M.R. \|last3=Schlunegger \|first3=F. \|last4=Norton \|first4=K.P. \|last5=Thomas \|first5=N. \|last6=Grindrod \|first6=P.M. \|last7=Chojnacki \|first7=M. \|bibcode=2016P&SS..121...36D \|url=https://boris.unibe.ch/74530/1/Diot_Schlunegger.pdf </ref> Researchers do not at this time understand how these features ere formed. .<ref>https://www.hou.usra.edu/meetings/lpsc2022/pdf/1588.pdf</ref> <ref>Cook, C., et al. 2022. FORMATION OF THE BANDED TERRAIN OF HELLAS PLANITIA, MARS. 53rd Lunar and Planetary Science Conference (2022). 1588.pdf</ref> Pictures of these features can look like abstract art.

← Older revision		Revision as of 19:08, 27 March 2020
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	==References==		==References==
	{{reflist\|colwidth=30em}}		{{reflist\|colwidth=30em}}
−
−	~~== External links ==~~
−	* https://www.youtube.com/watch?v=483HcpqyMNU Banded Flow Terrain in Hellas Basi