Elastic thickness estimates for coronae associated with chasmata on Venus
In this study we investigate the relationship between the local elastic lithospheric thickness and the relative ages of coronae on Venus in an attempt to further understand corona and chasmata formation/evolution. We use Magellan gravity and topography data to estimate the elastic lithospheric thick...
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| Veröffentlicht in: | Journal of Geophysical Research. E. Planets 2005-09, Vol.110 (E9), p.E09003.1-n/a |
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| creator | Hoogenboom, Trudi Houseman, Greg Martin, Paula |
| description | In this study we investigate the relationship between the local elastic lithospheric thickness and the relative ages of coronae on Venus in an attempt to further understand corona and chasmata formation/evolution. We use Magellan gravity and topography data to estimate the elastic lithospheric thickness in the vicinity of coronae associated with chasmata. The relative timing of corona formation with respect to chasmata formation is classified using superposition relationships between fractures and flows associated with the corona, and the regional fracture sets associated with the chasmata. For the 31 coronae that we here examine (limited by low resolution of the Magellan gravity field in some regions of interest), estimates of elastic thickness appear to be related to the relative timing of corona formation. Coronae that formed after chasmata exhibit smaller values of elastic thickness (0 to 19 km), which may result from their formation on relatively warm and weak lithosphere due to lithospheric extension associated with chasmata formation. Coronae that formed prior to chasmata formation display greater elastic thickness values (0 to 56 km). These coronae are interpreted to have formed on lithosphere that was stronger (colder). However, examples of coronae with small elastic thickness ( |
| doi_str_mv | 10.1029/2004JE002394 |
| format | Article |
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We use Magellan gravity and topography data to estimate the elastic lithospheric thickness in the vicinity of coronae associated with chasmata. The relative timing of corona formation with respect to chasmata formation is classified using superposition relationships between fractures and flows associated with the corona, and the regional fracture sets associated with the chasmata. For the 31 coronae that we here examine (limited by low resolution of the Magellan gravity field in some regions of interest), estimates of elastic thickness appear to be related to the relative timing of corona formation. Coronae that formed after chasmata exhibit smaller values of elastic thickness (0 to 19 km), which may result from their formation on relatively warm and weak lithosphere due to lithospheric extension associated with chasmata formation. Coronae that formed prior to chasmata formation display greater elastic thickness values (0 to 56 km). 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E. Planets</title><addtitle>J. Geophys. Res</addtitle><description>In this study we investigate the relationship between the local elastic lithospheric thickness and the relative ages of coronae on Venus in an attempt to further understand corona and chasmata formation/evolution. We use Magellan gravity and topography data to estimate the elastic lithospheric thickness in the vicinity of coronae associated with chasmata. The relative timing of corona formation with respect to chasmata formation is classified using superposition relationships between fractures and flows associated with the corona, and the regional fracture sets associated with the chasmata. For the 31 coronae that we here examine (limited by low resolution of the Magellan gravity field in some regions of interest), estimates of elastic thickness appear to be related to the relative timing of corona formation. Coronae that formed after chasmata exhibit smaller values of elastic thickness (0 to 19 km), which may result from their formation on relatively warm and weak lithosphere due to lithospheric extension associated with chasmata formation. Coronae that formed prior to chasmata formation display greater elastic thickness values (0 to 56 km). These coronae are interpreted to have formed on lithosphere that was stronger (colder). However, examples of coronae with small elastic thickness (<5 km) are found in all relative timing groups.</description><subject>admittance</subject><subject>chasmata</subject><subject>coronae</subject><subject>Coronas</subject><subject>Earth sciences</subject><subject>Earth, ocean, space</subject><subject>elastic</subject><subject>Estimates</subject><subject>Evolution</subject><subject>Exact sciences and technology</subject><subject>Fracture mechanics</subject><subject>Lithosphere</subject><subject>thickness</subject><subject>Time measurements</subject><subject>Topography</subject><subject>Venus</subject><issn>0148-0227</issn><issn>2169-9097</issn><issn>2156-2202</issn><issn>2169-9100</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2005</creationdate><recordtype>article</recordtype><recordid>eNqNkU1P20AQhlcVSI0oN37AXlr1gMvsl9c-VlGaEvFRVQF6W23Ga8XEsWHHEeXfd1GiwgmYy2hGz_tqPhg7EvBNgCxPJICeTQCkKvUHNpLC5JmUIPfYCIQuMpDSfmSHRLeQQptcgxix00nraWiQD8sGV10g4iHVaz8E4nUfOfax73zgnqjHJrUr_tAMS45LT4nyvO_4deg29Int176lcLjLB-zqx2Q-_pmdXU5Px9_PMjQCiqysdIloTFUVAAuwUhuotApW5roOCgXCQtTCaK-8R7AV5IBQFLkQoFGBOmBftr53sb_fpGHduiEMbeu70G_IySJtm3Z7BwgGSqXfBIXV1uTWJvDrG6ACKAsln6Y83qIYe6IYancX01XjoxPgnv7lXv4r4Z93zp7Qt3X0HTb0rLFSlMk9cXLLPTRteHzV082mvyeiNEUSZVtRQ0P4-1_k48rlVlnjbi6mzszV-fyXse6P-gfiBq-s</recordid><startdate>200509</startdate><enddate>200509</enddate><creator>Hoogenboom, Trudi</creator><creator>Houseman, Greg</creator><creator>Martin, Paula</creator><general>Blackwell Publishing Ltd</general><general>American Geophysical Union</general><scope>BSCLL</scope><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope><scope>7U5</scope><scope>FR3</scope><scope>KR7</scope></search><sort><creationdate>200509</creationdate><title>Elastic thickness estimates for coronae associated with chasmata on Venus</title><author>Hoogenboom, Trudi ; Houseman, Greg ; Martin, Paula</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c5108-9d49cc55dd800b072450d43e7264fe3c1c0b1f154a3aac07d060c08861104c303</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2005</creationdate><topic>admittance</topic><topic>chasmata</topic><topic>coronae</topic><topic>Coronas</topic><topic>Earth sciences</topic><topic>Earth, ocean, space</topic><topic>elastic</topic><topic>Estimates</topic><topic>Evolution</topic><topic>Exact sciences and technology</topic><topic>Fracture mechanics</topic><topic>Lithosphere</topic><topic>thickness</topic><topic>Time measurements</topic><topic>Topography</topic><topic>Venus</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Hoogenboom, Trudi</creatorcontrib><creatorcontrib>Houseman, Greg</creatorcontrib><creatorcontrib>Martin, Paula</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Solid State and Superconductivity Abstracts</collection><collection>Engineering Research Database</collection><collection>Civil Engineering Abstracts</collection><jtitle>Journal of Geophysical Research. E. Planets</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Hoogenboom, Trudi</au><au>Houseman, Greg</au><au>Martin, Paula</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Elastic thickness estimates for coronae associated with chasmata on Venus</atitle><jtitle>Journal of Geophysical Research. E. Planets</jtitle><addtitle>J. Geophys. Res</addtitle><date>2005-09</date><risdate>2005</risdate><volume>110</volume><issue>E9</issue><spage>E09003.1</spage><epage>n/a</epage><pages>E09003.1-n/a</pages><issn>0148-0227</issn><issn>2169-9097</issn><eissn>2156-2202</eissn><eissn>2169-9100</eissn><abstract>In this study we investigate the relationship between the local elastic lithospheric thickness and the relative ages of coronae on Venus in an attempt to further understand corona and chasmata formation/evolution. We use Magellan gravity and topography data to estimate the elastic lithospheric thickness in the vicinity of coronae associated with chasmata. The relative timing of corona formation with respect to chasmata formation is classified using superposition relationships between fractures and flows associated with the corona, and the regional fracture sets associated with the chasmata. For the 31 coronae that we here examine (limited by low resolution of the Magellan gravity field in some regions of interest), estimates of elastic thickness appear to be related to the relative timing of corona formation. Coronae that formed after chasmata exhibit smaller values of elastic thickness (0 to 19 km), which may result from their formation on relatively warm and weak lithosphere due to lithospheric extension associated with chasmata formation. Coronae that formed prior to chasmata formation display greater elastic thickness values (0 to 56 km). These coronae are interpreted to have formed on lithosphere that was stronger (colder). However, examples of coronae with small elastic thickness (<5 km) are found in all relative timing groups.</abstract><cop>Washington, DC</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/2004JE002394</doi><tpages>9</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | admittance chasmata coronae Coronas Earth sciences Earth, ocean, space elastic Estimates Evolution Exact sciences and technology Fracture mechanics Lithosphere thickness Time measurements Topography Venus |
| title | Elastic thickness estimates for coronae associated with chasmata on Venus |
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