Distribution of Early, Middle, and Late Noachian cratered surfaces in the Martian highlands: Implications for resurfacing events and processes
Most of the geomorphic changes on Mars occurred during the Noachian Period, when the rates of impact crater degradation and valley network incision were highest. Fluvial erosion around the Noachian/Hesperian transition is better constrained than the longer‐term landscape evolution throughout the Noa...
Gespeichert in:
Veröffentlicht in: | Journal of geophysical research. Planets 2013-02, Vol.118 (2), p.278-291 |
---|---|
Hauptverfasser: | , , |
Format: | Artikel |
Sprache: | eng |
Schlagworte: | |
Online-Zugang: | Volltext |
Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
container_end_page | 291 |
---|---|
container_issue | 2 |
container_start_page | 278 |
container_title | Journal of geophysical research. Planets |
container_volume | 118 |
creator | Irwin III, Rossman P. Tanaka, Kenneth L. Robbins, Stuart J. |
description | Most of the geomorphic changes on Mars occurred during the Noachian Period, when the rates of impact crater degradation and valley network incision were highest. Fluvial erosion around the Noachian/Hesperian transition is better constrained than the longer‐term landscape evolution throughout the Noachian Period, when the highland intercrater geomorphic surfaces developed. We interpret highland resurfacing events and processes using a new global geologic map of Mars (at 1:20,000,000 scale), a crater data set that is complete down to 1 km in diameter, and Mars Orbiter Laser Altimeter topography. The Early Noachian highland (eNh) unit is nearly saturated with craters of 32–128 km diameter, the Middle Noachian highland (mNh) unit has a resurfacing age of ~4 Ga, and the Late Noachian highland unit (lNh) includes younger composite surfaces of basin fill and partially buried cratered terrain. These units have statistically distinct ages, and their distribution varies with elevation. The eNh unit is concentrated in the high‐standing Hellas basin annulus and in highland terrain that was thinly mantled by basin ejecta near 180° longitude. The mNh unit includes most of Arabia Terra, the Argyre vicinity, highland plateau areas between eNh outcrops, and the Thaumasia range. The lNh unit mostly occurs within highland basins. Crater depth/diameter ratios do not vary strongly between the eNh and mNh units, although crater losses to Noachian resurfacing appear greater in lower lying areas. Noachian resurfacing was spatially non‐uniform, long‐lived, and gravity‐driven, more consistent with arid‐zone fluvial and aeolian erosion and volcanism than with air fall mantling or mass wasting.
Key Points
The Early Noachian highland unit is nearly saturated with 32‐128 km craters.
Noachian resurfacing depended on regional and topographic location.
Resurfacing likely included fluvial, aeolian, and volcanic processes. |
doi_str_mv | 10.1002/jgre.20053 |
format | Article |
fullrecord | <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_proquest_miscellaneous_1559655668</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>1559655668</sourcerecordid><originalsourceid>FETCH-LOGICAL-a4973-16156c512e014f5563fef50caec093f2b44d318a446bd7fac81722ab9ea36963</originalsourceid><addsrcrecordid>eNp9kcFO4zAURSM0SCBgwxdYYjNCBOw4duLZIVoKqBSBKmBnuc5z65ImxU6A_gTfjEuABYvxxvbTufc-6UbRPsHHBOPkZD51cJxgzOhGtJ0QLmIR5n--31hkW9Ge93McTh5GhG5H7z3rG2cnbWPrCtUG9ZUrV0fo2hZFCUdIVQUaqgbQqFZ6ZlWFtAtfBwXyrTNKg0e2Qs0M0LVyzRqY2emsDDr_D10ulqXVau3tkakdctCpbDVF8AJV4z8Tlq4ORh78brRpVOlh7-veicbn_fHZRTy8GVyenQ5jlYqMxoQTxjUjCWCSGsY4NWAY1go0FtQkkzQtKMlVmvJJkYW8nGRJoiYCFOWC053ob2cbgp9b8I1cWK-hDGtD3XpJGBM82PI8oAe_0HnduiosJwmneYo5FiJQhx2lXe29AyOXzi6UW0mC5bocuS5HfpYTYNLBr7aE1X9IeTW4639r4k4T6oK3H41yT5JnNGPyYTSQ97079ji6pXJMPwAOkqGv</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>1638406099</pqid></control><display><type>article</type><title>Distribution of Early, Middle, and Late Noachian cratered surfaces in the Martian highlands: Implications for resurfacing events and processes</title><source>Wiley Online Library Journals Frontfile Complete</source><source>Wiley Free Content</source><source>Alma/SFX Local Collection</source><creator>Irwin III, Rossman P. ; Tanaka, Kenneth L. ; Robbins, Stuart J.</creator><creatorcontrib>Irwin III, Rossman P. ; Tanaka, Kenneth L. ; Robbins, Stuart J.</creatorcontrib><description>Most of the geomorphic changes on Mars occurred during the Noachian Period, when the rates of impact crater degradation and valley network incision were highest. Fluvial erosion around the Noachian/Hesperian transition is better constrained than the longer‐term landscape evolution throughout the Noachian Period, when the highland intercrater geomorphic surfaces developed. We interpret highland resurfacing events and processes using a new global geologic map of Mars (at 1:20,000,000 scale), a crater data set that is complete down to 1 km in diameter, and Mars Orbiter Laser Altimeter topography. The Early Noachian highland (eNh) unit is nearly saturated with craters of 32–128 km diameter, the Middle Noachian highland (mNh) unit has a resurfacing age of ~4 Ga, and the Late Noachian highland unit (lNh) includes younger composite surfaces of basin fill and partially buried cratered terrain. These units have statistically distinct ages, and their distribution varies with elevation. The eNh unit is concentrated in the high‐standing Hellas basin annulus and in highland terrain that was thinly mantled by basin ejecta near 180° longitude. The mNh unit includes most of Arabia Terra, the Argyre vicinity, highland plateau areas between eNh outcrops, and the Thaumasia range. The lNh unit mostly occurs within highland basins. Crater depth/diameter ratios do not vary strongly between the eNh and mNh units, although crater losses to Noachian resurfacing appear greater in lower lying areas. Noachian resurfacing was spatially non‐uniform, long‐lived, and gravity‐driven, more consistent with arid‐zone fluvial and aeolian erosion and volcanism than with air fall mantling or mass wasting.
Key Points
The Early Noachian highland unit is nearly saturated with 32‐128 km craters.
Noachian resurfacing depended on regional and topographic location.
Resurfacing likely included fluvial, aeolian, and volcanic processes.</description><identifier>ISSN: 2169-9097</identifier><identifier>EISSN: 2169-9100</identifier><identifier>DOI: 10.1002/jgre.20053</identifier><language>eng</language><publisher>Washington: Blackwell Publishing Ltd</publisher><subject>cratering ; Geologic mapping ; highland ; Mars ; Mass wasting ; resurfacing</subject><ispartof>Journal of geophysical research. Planets, 2013-02, Vol.118 (2), p.278-291</ispartof><rights>2013. American Geophysical Union. All Rights Reserved.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-a4973-16156c512e014f5563fef50caec093f2b44d318a446bd7fac81722ab9ea36963</citedby><cites>FETCH-LOGICAL-a4973-16156c512e014f5563fef50caec093f2b44d318a446bd7fac81722ab9ea36963</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1002%2Fjgre.20053$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1002%2Fjgre.20053$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>314,776,780,1411,1427,27903,27904,45553,45554,46387,46811</link.rule.ids></links><search><creatorcontrib>Irwin III, Rossman P.</creatorcontrib><creatorcontrib>Tanaka, Kenneth L.</creatorcontrib><creatorcontrib>Robbins, Stuart J.</creatorcontrib><title>Distribution of Early, Middle, and Late Noachian cratered surfaces in the Martian highlands: Implications for resurfacing events and processes</title><title>Journal of geophysical research. Planets</title><addtitle>J. Geophys. Res. Planets</addtitle><description>Most of the geomorphic changes on Mars occurred during the Noachian Period, when the rates of impact crater degradation and valley network incision were highest. Fluvial erosion around the Noachian/Hesperian transition is better constrained than the longer‐term landscape evolution throughout the Noachian Period, when the highland intercrater geomorphic surfaces developed. We interpret highland resurfacing events and processes using a new global geologic map of Mars (at 1:20,000,000 scale), a crater data set that is complete down to 1 km in diameter, and Mars Orbiter Laser Altimeter topography. The Early Noachian highland (eNh) unit is nearly saturated with craters of 32–128 km diameter, the Middle Noachian highland (mNh) unit has a resurfacing age of ~4 Ga, and the Late Noachian highland unit (lNh) includes younger composite surfaces of basin fill and partially buried cratered terrain. These units have statistically distinct ages, and their distribution varies with elevation. The eNh unit is concentrated in the high‐standing Hellas basin annulus and in highland terrain that was thinly mantled by basin ejecta near 180° longitude. The mNh unit includes most of Arabia Terra, the Argyre vicinity, highland plateau areas between eNh outcrops, and the Thaumasia range. The lNh unit mostly occurs within highland basins. Crater depth/diameter ratios do not vary strongly between the eNh and mNh units, although crater losses to Noachian resurfacing appear greater in lower lying areas. Noachian resurfacing was spatially non‐uniform, long‐lived, and gravity‐driven, more consistent with arid‐zone fluvial and aeolian erosion and volcanism than with air fall mantling or mass wasting.
Key Points
The Early Noachian highland unit is nearly saturated with 32‐128 km craters.
Noachian resurfacing depended on regional and topographic location.
Resurfacing likely included fluvial, aeolian, and volcanic processes.</description><subject>cratering</subject><subject>Geologic mapping</subject><subject>highland</subject><subject>Mars</subject><subject>Mass wasting</subject><subject>resurfacing</subject><issn>2169-9097</issn><issn>2169-9100</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><recordid>eNp9kcFO4zAURSM0SCBgwxdYYjNCBOw4duLZIVoKqBSBKmBnuc5z65ImxU6A_gTfjEuABYvxxvbTufc-6UbRPsHHBOPkZD51cJxgzOhGtJ0QLmIR5n--31hkW9Ge93McTh5GhG5H7z3rG2cnbWPrCtUG9ZUrV0fo2hZFCUdIVQUaqgbQqFZ6ZlWFtAtfBwXyrTNKg0e2Qs0M0LVyzRqY2emsDDr_D10ulqXVau3tkakdctCpbDVF8AJV4z8Tlq4ORh78brRpVOlh7-veicbn_fHZRTy8GVyenQ5jlYqMxoQTxjUjCWCSGsY4NWAY1go0FtQkkzQtKMlVmvJJkYW8nGRJoiYCFOWC053ob2cbgp9b8I1cWK-hDGtD3XpJGBM82PI8oAe_0HnduiosJwmneYo5FiJQhx2lXe29AyOXzi6UW0mC5bocuS5HfpYTYNLBr7aE1X9IeTW4639r4k4T6oK3H41yT5JnNGPyYTSQ97079ji6pXJMPwAOkqGv</recordid><startdate>201302</startdate><enddate>201302</enddate><creator>Irwin III, Rossman P.</creator><creator>Tanaka, Kenneth L.</creator><creator>Robbins, Stuart J.</creator><general>Blackwell Publishing Ltd</general><scope>BSCLL</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope></search><sort><creationdate>201302</creationdate><title>Distribution of Early, Middle, and Late Noachian cratered surfaces in the Martian highlands: Implications for resurfacing events and processes</title><author>Irwin III, Rossman P. ; Tanaka, Kenneth L. ; Robbins, Stuart J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a4973-16156c512e014f5563fef50caec093f2b44d318a446bd7fac81722ab9ea36963</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>cratering</topic><topic>Geologic mapping</topic><topic>highland</topic><topic>Mars</topic><topic>Mass wasting</topic><topic>resurfacing</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Irwin III, Rossman P.</creatorcontrib><creatorcontrib>Tanaka, Kenneth L.</creatorcontrib><creatorcontrib>Robbins, Stuart J.</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Journal of geophysical research. Planets</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Irwin III, Rossman P.</au><au>Tanaka, Kenneth L.</au><au>Robbins, Stuart J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Distribution of Early, Middle, and Late Noachian cratered surfaces in the Martian highlands: Implications for resurfacing events and processes</atitle><jtitle>Journal of geophysical research. Planets</jtitle><addtitle>J. Geophys. Res. Planets</addtitle><date>2013-02</date><risdate>2013</risdate><volume>118</volume><issue>2</issue><spage>278</spage><epage>291</epage><pages>278-291</pages><issn>2169-9097</issn><eissn>2169-9100</eissn><abstract>Most of the geomorphic changes on Mars occurred during the Noachian Period, when the rates of impact crater degradation and valley network incision were highest. Fluvial erosion around the Noachian/Hesperian transition is better constrained than the longer‐term landscape evolution throughout the Noachian Period, when the highland intercrater geomorphic surfaces developed. We interpret highland resurfacing events and processes using a new global geologic map of Mars (at 1:20,000,000 scale), a crater data set that is complete down to 1 km in diameter, and Mars Orbiter Laser Altimeter topography. The Early Noachian highland (eNh) unit is nearly saturated with craters of 32–128 km diameter, the Middle Noachian highland (mNh) unit has a resurfacing age of ~4 Ga, and the Late Noachian highland unit (lNh) includes younger composite surfaces of basin fill and partially buried cratered terrain. These units have statistically distinct ages, and their distribution varies with elevation. The eNh unit is concentrated in the high‐standing Hellas basin annulus and in highland terrain that was thinly mantled by basin ejecta near 180° longitude. The mNh unit includes most of Arabia Terra, the Argyre vicinity, highland plateau areas between eNh outcrops, and the Thaumasia range. The lNh unit mostly occurs within highland basins. Crater depth/diameter ratios do not vary strongly between the eNh and mNh units, although crater losses to Noachian resurfacing appear greater in lower lying areas. Noachian resurfacing was spatially non‐uniform, long‐lived, and gravity‐driven, more consistent with arid‐zone fluvial and aeolian erosion and volcanism than with air fall mantling or mass wasting.
Key Points
The Early Noachian highland unit is nearly saturated with 32‐128 km craters.
Noachian resurfacing depended on regional and topographic location.
Resurfacing likely included fluvial, aeolian, and volcanic processes.</abstract><cop>Washington</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1002/jgre.20053</doi><tpages>14</tpages><oa>free_for_read</oa></addata></record> |
fulltext | fulltext |
identifier | ISSN: 2169-9097 |
ispartof | Journal of geophysical research. Planets, 2013-02, Vol.118 (2), p.278-291 |
issn | 2169-9097 2169-9100 |
language | eng |
recordid | cdi_proquest_miscellaneous_1559655668 |
source | Wiley Online Library Journals Frontfile Complete; Wiley Free Content; Alma/SFX Local Collection |
subjects | cratering Geologic mapping highland Mars Mass wasting resurfacing |
title | Distribution of Early, Middle, and Late Noachian cratered surfaces in the Martian highlands: Implications for resurfacing events and processes |
url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-25T19%3A21%3A29IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Distribution%20of%20Early,%20Middle,%20and%20Late%20Noachian%20cratered%20surfaces%20in%20the%20Martian%20highlands:%20Implications%20for%20resurfacing%20events%20and%20processes&rft.jtitle=Journal%20of%20geophysical%20research.%20Planets&rft.au=Irwin%20III,%20Rossman%20P.&rft.date=2013-02&rft.volume=118&rft.issue=2&rft.spage=278&rft.epage=291&rft.pages=278-291&rft.issn=2169-9097&rft.eissn=2169-9100&rft_id=info:doi/10.1002/jgre.20053&rft_dat=%3Cproquest_cross%3E1559655668%3C/proquest_cross%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=1638406099&rft_id=info:pmid/&rfr_iscdi=true |