MozartV1, PascalFrancis, Corpus, bibRecord, 000016

The origin of graben and ridges in Rachmaninoff, Raditladi, and Mozart basins, Mercury

Identifieur interne : 000016 ( PascalFrancis/Corpus ); précédent : 000015; suivant : 000017

The origin of graben and ridges in Rachmaninoff, Raditladi, and Mozart basins, Mercury

Auteurs : David M. Blair ; Andrew M. Freed ; Paul K. Byrne ; Christian Klimczak ; Louise M. Prockter ; Carolyn M. Ernst ; Sean C. Solomon ; H. Jay Melosh ; Maria T. Zuber

Source :

Journal of geophysical research. Planets [ 2169-9097 ] ; 2013.

RBID : Pascal:13-0353144

Descripteurs français

Pascal (Inist)
- Graben, Mercure, Tectonique, Forme relief, Orientation, Méthode élément fini, Modèle, Contraction, Plaine, Surrection, Bassin subsidence, Subsidence, Monde, Ecoulement, Matériau, Mise en place, Refroidissement, Lave, Viscosité, Epaisseur, Cratère.

English descriptors

KwdEn :
- contraction, cooling, craters, emplacement, finite element analysis, flow, global, grabens, landforms, lava, materials, mercury, models, orientation, plains, subsidence, subsidence basins, tectonics, thickness, uplifts, viscosity.

Abstract

The Rachmaninoff, Raditladi, and Mozart peak-ring impact basins on Mercury display a distinctive pattern of tectonic features consisting of a central zone that is either devoid of tectonic landforms or contains small ridges, a medial annulus of prominent and predominantly circumferentially oriented graben, and a distal zone displaying graben that occur in a mix of orientations and that are less evident toward the peak ring. Here we use finite element models to explore three candidate scenarios for the formation of these tectonic features: (1) thermal contraction of the interior smooth plains, (2) isostatic uplift of the basin floor, and (3) subsidence following volcanic loading. Our results suggest that only thermal contraction can account for the observed pattern of graben, whereas some combination of subsidence and global contraction is the most likely explanation for the central ridges in Rachmaninoff and Mozart. Thermal contraction models, however, predict the formation of graben in the centermost region of each basin, where no graben are observed. We hypothesize that graben in this region were buried by a thin, late-stage flow of plains material, and images of partially filled graben provide evidence of such late-stage plains emplacement. These results suggest that the smooth plains units in these three basins are volcanic in origin. The thermal contraction models also imply a cooling unit ∼1 km thick near the basin center, further supporting the view that plains-forming lavas on Mercury were often of sufficiently high volume and low viscosity to pool to substantial thicknesses within basins and craters.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A08	`01`	`1`	`ENG`	`@1 The origin of graben and ridges in Rachmaninoff, Raditladi, and Mozart basins, Mercury`
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A11	`02`	`1`		`@1 FREED (Andrew M.)`
A11	`03`	`1`		`@1 BYRNE (Paul K.)`
A11	`04`	`1`		`@1 KLIMCZAK (Christian)`
A11	`05`	`1`		`@1 PROCKTER (Louise M.)`
A11	`06`	`1`		`@1 ERNST (Carolyn M.)`
A11	`07`	`1`		`@1 SOLOMON (Sean C.)`
A11	`08`	`1`		`@1 MELOSH (H. Jay)`
A11	`09`	`1`		`@1 ZUBER (Maria T.)`
A14	`01`			`@1 Department of Earth, Atmospheric, and Planetary Sciences, Purdue University @2 West Lafayette, Indiana @3 USA @Z 1 aut. @Z 2 aut. @Z 8 aut.`
A14	`02`			`@1 Department of Terrestrial Magnetism, Carnegie Institution of Washington, NW @2 Washington, DC @3 USA @Z 3 aut. @Z 4 aut. @Z 7 aut.`
A14	`03`			`@1 The Johns Hopkins University Applied Physics Laboratory @2 Laurel, Maryland @3 USA @Z 5 aut. @Z 6 aut.`
A14	`04`			`@1 Lamont-Doherty Earth Observatory, Columbia University @2 Palisades, New York @3 USA @Z 7 aut.`
A14	`05`			`@1 Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology @2 Cambridge, Massachusetts @3 USA @Z 9 aut.`
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C01	`01`		`ENG`	@0 The Rachmaninoff, Raditladi, and Mozart peak-ring impact basins on Mercury display a distinctive pattern of tectonic features consisting of a central zone that is either devoid of tectonic landforms or contains small ridges, a medial annulus of prominent and predominantly circumferentially oriented graben, and a distal zone displaying graben that occur in a mix of orientations and that are less evident toward the peak ring. Here we use finite element models to explore three candidate scenarios for the formation of these tectonic features: (1) thermal contraction of the interior smooth plains, (2) isostatic uplift of the basin floor, and (3) subsidence following volcanic loading. Our results suggest that only thermal contraction can account for the observed pattern of graben, whereas some combination of subsidence and global contraction is the most likely explanation for the central ridges in Rachmaninoff and Mozart. Thermal contraction models, however, predict the formation of graben in the centermost region of each basin, where no graben are observed. We hypothesize that graben in this region were buried by a thin, late-stage flow of plains material, and images of partially filled graben provide evidence of such late-stage plains emplacement. These results suggest that the smooth plains units in these three basins are volcanic in origin. The thermal contraction models also imply a cooling unit ∼1 km thick near the basin center, further supporting the view that plains-forming lavas on Mercury were often of sufficiently high volume and low viscosity to pool to substantial thicknesses within basins and craters.
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N21				`@1 336`

Format Inist (serveur)

NO :	PASCAL 13-0353144 INIST
ET :	The origin of graben and ridges in Rachmaninoff, Raditladi, and Mozart basins, Mercury
AU :	BLAIR (David M.); FREED (Andrew M.); BYRNE (Paul K.); KLIMCZAK (Christian); PROCKTER (Louise M.); ERNST (Carolyn M.); SOLOMON (Sean C.); MELOSH (H. Jay); ZUBER (Maria T.)
AF :	Department of Earth, Atmospheric, and Planetary Sciences, Purdue University/West Lafayette, Indiana/Etats-Unis (1 aut., 2 aut., 8 aut.); Department of Terrestrial Magnetism, Carnegie Institution of Washington, NW/Washington, DC/Etats-Unis (3 aut., 4 aut., 7 aut.); The Johns Hopkins University Applied Physics Laboratory/Laurel, Maryland/Etats-Unis (5 aut., 6 aut.); Lamont-Doherty Earth Observatory, Columbia University/Palisades, New York/Etats-Unis (7 aut.); Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology/Cambridge, Massachusetts/Etats-Unis (9 aut.)
DT :	Publication en série; Niveau analytique
SO :	Journal of geophysical research. Planets; ISSN 2169-9097; Etats-Unis; Da. 2013; Vol. 118; No. 1; Pp. 47-58; Bibl. 1 p.1/4
LA :	Anglais
EA :	The Rachmaninoff, Raditladi, and Mozart peak-ring impact basins on Mercury display a distinctive pattern of tectonic features consisting of a central zone that is either devoid of tectonic landforms or contains small ridges, a medial annulus of prominent and predominantly circumferentially oriented graben, and a distal zone displaying graben that occur in a mix of orientations and that are less evident toward the peak ring. Here we use finite element models to explore three candidate scenarios for the formation of these tectonic features: (1) thermal contraction of the interior smooth plains, (2) isostatic uplift of the basin floor, and (3) subsidence following volcanic loading. Our results suggest that only thermal contraction can account for the observed pattern of graben, whereas some combination of subsidence and global contraction is the most likely explanation for the central ridges in Rachmaninoff and Mozart. Thermal contraction models, however, predict the formation of graben in the centermost region of each basin, where no graben are observed. We hypothesize that graben in this region were buried by a thin, late-stage flow of plains material, and images of partially filled graben provide evidence of such late-stage plains emplacement. These results suggest that the smooth plains units in these three basins are volcanic in origin. The thermal contraction models also imply a cooling unit ∼1 km thick near the basin center, further supporting the view that plains-forming lavas on Mercury were often of sufficiently high volume and low viscosity to pool to substantial thicknesses within basins and craters.
CC :	001E01; 220
FD :	Graben; Mercure; Tectonique; Forme relief; Orientation; Méthode élément fini; Modèle; Contraction; Plaine; Surrection; Bassin subsidence; Subsidence; Monde; Ecoulement; Matériau; Mise en place; Refroidissement; Lave; Viscosité; Epaisseur; Cratère
ED :	grabens; mercury; tectonics; landforms; orientation; finite element analysis; models; contraction; plains; uplifts; subsidence basins; subsidence; global; flow; materials; emplacement; cooling; lava; viscosity; thickness; craters
SD :	Graben; Mercurio; Tectónico; Orientación; Modelo; Contracción; Llano; Cuenca de subsidencia; Subsidencia; Mundo; Emplazamiento; Enfriamiento; Lava; Viscosidad; Espesor; Cráter
LO :	INIST-3144E1.354000140724260050
ID :	13-0353144

Links to Exploration step

Pascal:13-0353144

Le document en format XML

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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>contraction</term>
<term>cooling</term>
<term>craters</term>
<term>emplacement</term>
<term>finite element analysis</term>
<term>flow</term>
<term>global</term>
<term>grabens</term>
<term>landforms</term>
<term>lava</term>
<term>materials</term>
<term>mercury</term>
<term>models</term>
<term>orientation</term>
<term>plains</term>
<term>subsidence</term>
<term>subsidence basins</term>
<term>tectonics</term>
<term>thickness</term>
<term>uplifts</term>
<term>viscosity</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Graben</term>
<term>Mercure</term>
<term>Tectonique</term>
<term>Forme relief</term>
<term>Orientation</term>
<term>Méthode élément fini</term>
<term>Modèle</term>
<term>Contraction</term>
<term>Plaine</term>
<term>Surrection</term>
<term>Bassin subsidence</term>
<term>Subsidence</term>
<term>Monde</term>
<term>Ecoulement</term>
<term>Matériau</term>
<term>Mise en place</term>
<term>Refroidissement</term>
<term>Lave</term>
<term>Viscosité</term>
<term>Epaisseur</term>
<term>Cratère</term>
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<front><div type="abstract" xml:lang="en">The Rachmaninoff, Raditladi, and Mozart peak-ring impact basins on Mercury display a distinctive pattern of tectonic features consisting of a central zone that is either devoid of tectonic landforms or contains small ridges, a medial annulus of prominent and predominantly circumferentially oriented graben, and a distal zone displaying graben that occur in a mix of orientations and that are less evident toward the peak ring. Here we use finite element models to explore three candidate scenarios for the formation of these tectonic features: (1) thermal contraction of the interior smooth plains, (2) isostatic uplift of the basin floor, and (3) subsidence following volcanic loading. Our results suggest that only thermal contraction can account for the observed pattern of graben, whereas some combination of subsidence and global contraction is the most likely explanation for the central ridges in Rachmaninoff and Mozart. Thermal contraction models, however, predict the formation of graben in the centermost region of each basin, where no graben are observed. We hypothesize that graben in this region were buried by a thin, late-stage flow of plains material, and images of partially filled graben provide evidence of such late-stage plains emplacement. These results suggest that the smooth plains units in these three basins are volcanic in origin. The thermal contraction models also imply a cooling unit ∼1 km thick near the basin center, further supporting the view that plains-forming lavas on Mercury were often of sufficiently high volume and low viscosity to pool to substantial thicknesses within basins and craters.</div>
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<fA08 i1="01" i2="1" l="ENG"><s1>The origin of graben and ridges in Rachmaninoff, Raditladi, and Mozart basins, Mercury</s1>
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<fA11 i1="02" i2="1"><s1>FREED (Andrew M.)</s1>
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<fA11 i1="09" i2="1"><s1>ZUBER (Maria T.)</s1>
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<fA14 i1="01"><s1>Department of Earth, Atmospheric, and Planetary Sciences, Purdue University</s1>
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<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
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<fA14 i1="02"><s1>Department of Terrestrial Magnetism, Carnegie Institution of Washington, NW</s1>
<s2>Washington, DC</s2>
<s3>USA</s3>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
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<fA14 i1="03"><s1>The Johns Hopkins University Applied Physics Laboratory</s1>
<s2>Laurel, Maryland</s2>
<s3>USA</s3>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
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<fA14 i1="04"><s1>Lamont-Doherty Earth Observatory, Columbia University</s1>
<s2>Palisades, New York</s2>
<s3>USA</s3>
<sZ>7 aut.</sZ>
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<fA14 i1="05"><s1>Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology</s1>
<s2>Cambridge, Massachusetts</s2>
<s3>USA</s3>
<sZ>9 aut.</sZ>
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<fA21><s1>2013</s1>
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<fC01 i1="01" l="ENG"><s0>The Rachmaninoff, Raditladi, and Mozart peak-ring impact basins on Mercury display a distinctive pattern of tectonic features consisting of a central zone that is either devoid of tectonic landforms or contains small ridges, a medial annulus of prominent and predominantly circumferentially oriented graben, and a distal zone displaying graben that occur in a mix of orientations and that are less evident toward the peak ring. Here we use finite element models to explore three candidate scenarios for the formation of these tectonic features: (1) thermal contraction of the interior smooth plains, (2) isostatic uplift of the basin floor, and (3) subsidence following volcanic loading. Our results suggest that only thermal contraction can account for the observed pattern of graben, whereas some combination of subsidence and global contraction is the most likely explanation for the central ridges in Rachmaninoff and Mozart. Thermal contraction models, however, predict the formation of graben in the centermost region of each basin, where no graben are observed. We hypothesize that graben in this region were buried by a thin, late-stage flow of plains material, and images of partially filled graben provide evidence of such late-stage plains emplacement. These results suggest that the smooth plains units in these three basins are volcanic in origin. The thermal contraction models also imply a cooling unit ∼1 km thick near the basin center, further supporting the view that plains-forming lavas on Mercury were often of sufficiently high volume and low viscosity to pool to substantial thicknesses within basins and craters.</s0>
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<fC03 i1="01" i2="2" l="FRE"><s0>Graben</s0>
<s5>01</s5>
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<fC03 i1="01" i2="2" l="ENG"><s0>grabens</s0>
<s5>01</s5>
</fC03>
<fC03 i1="01" i2="2" l="SPA"><s0>Graben</s0>
<s5>01</s5>
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<fC03 i1="02" i2="2" l="FRE"><s0>Mercure</s0>
<s5>02</s5>
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<fC03 i1="02" i2="2" l="ENG"><s0>mercury</s0>
<s5>02</s5>
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<fC03 i1="02" i2="2" l="SPA"><s0>Mercurio</s0>
<s5>02</s5>
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<fC03 i1="03" i2="2" l="FRE"><s0>Tectonique</s0>
<s5>03</s5>
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<fC03 i1="03" i2="2" l="ENG"><s0>tectonics</s0>
<s5>03</s5>
</fC03>
<fC03 i1="03" i2="2" l="SPA"><s0>Tectónico</s0>
<s5>03</s5>
</fC03>
<fC03 i1="04" i2="2" l="FRE"><s0>Forme relief</s0>
<s5>04</s5>
</fC03>
<fC03 i1="04" i2="2" l="ENG"><s0>landforms</s0>
<s5>04</s5>
</fC03>
<fC03 i1="05" i2="2" l="FRE"><s0>Orientation</s0>
<s5>05</s5>
</fC03>
<fC03 i1="05" i2="2" l="ENG"><s0>orientation</s0>
<s5>05</s5>
</fC03>
<fC03 i1="05" i2="2" l="SPA"><s0>Orientación</s0>
<s5>05</s5>
</fC03>
<fC03 i1="06" i2="2" l="FRE"><s0>Méthode élément fini</s0>
<s5>06</s5>
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<fC03 i1="06" i2="2" l="ENG"><s0>finite element analysis</s0>
<s5>06</s5>
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<fC03 i1="07" i2="2" l="FRE"><s0>Modèle</s0>
<s5>07</s5>
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<fC03 i1="07" i2="2" l="ENG"><s0>models</s0>
<s5>07</s5>
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<fC03 i1="07" i2="2" l="SPA"><s0>Modelo</s0>
<s5>07</s5>
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<fC03 i1="08" i2="2" l="FRE"><s0>Contraction</s0>
<s5>08</s5>
</fC03>
<fC03 i1="08" i2="2" l="ENG"><s0>contraction</s0>
<s5>08</s5>
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<fC03 i1="08" i2="2" l="SPA"><s0>Contracción</s0>
<s5>08</s5>
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<fC03 i1="09" i2="2" l="FRE"><s0>Plaine</s0>
<s5>09</s5>
</fC03>
<fC03 i1="09" i2="2" l="ENG"><s0>plains</s0>
<s5>09</s5>
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<fC03 i1="09" i2="2" l="SPA"><s0>Llano</s0>
<s5>09</s5>
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<fC03 i1="10" i2="2" l="FRE"><s0>Surrection</s0>
<s5>10</s5>
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<fC03 i1="10" i2="2" l="ENG"><s0>uplifts</s0>
<s5>10</s5>
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<fC03 i1="11" i2="2" l="FRE"><s0>Bassin subsidence</s0>
<s5>11</s5>
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<fC03 i1="11" i2="2" l="ENG"><s0>subsidence basins</s0>
<s5>11</s5>
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<fC03 i1="11" i2="2" l="SPA"><s0>Cuenca de subsidencia</s0>
<s5>11</s5>
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<fC03 i1="12" i2="2" l="FRE"><s0>Subsidence</s0>
<s5>13</s5>
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<fC03 i1="12" i2="2" l="ENG"><s0>subsidence</s0>
<s5>13</s5>
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<fC03 i1="12" i2="2" l="SPA"><s0>Subsidencia</s0>
<s5>13</s5>
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<fC03 i1="13" i2="2" l="FRE"><s0>Monde</s0>
<s5>14</s5>
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<s5>14</s5>
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<fC03 i1="13" i2="2" l="SPA"><s0>Mundo</s0>
<s5>14</s5>
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<fC03 i1="14" i2="2" l="FRE"><s0>Ecoulement</s0>
<s5>15</s5>
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<s5>15</s5>
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<s5>16</s5>
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<fC03 i1="16" i2="2" l="FRE"><s0>Mise en place</s0>
<s5>17</s5>
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<fC03 i1="16" i2="2" l="ENG"><s0>emplacement</s0>
<s5>17</s5>
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<fC03 i1="16" i2="2" l="SPA"><s0>Emplazamiento</s0>
<s5>17</s5>
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<fC03 i1="17" i2="2" l="FRE"><s0>Refroidissement</s0>
<s5>18</s5>
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<fC03 i1="17" i2="2" l="ENG"><s0>cooling</s0>
<s5>18</s5>
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<fC03 i1="17" i2="2" l="SPA"><s0>Enfriamiento</s0>
<s5>18</s5>
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<fC03 i1="18" i2="2" l="FRE"><s0>Lave</s0>
<s5>19</s5>
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<fC03 i1="18" i2="2" l="ENG"><s0>lava</s0>
<s5>19</s5>
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<fC03 i1="18" i2="2" l="SPA"><s0>Lava</s0>
<s5>19</s5>
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<fC03 i1="19" i2="2" l="FRE"><s0>Viscosité</s0>
<s5>20</s5>
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<fC03 i1="19" i2="2" l="ENG"><s0>viscosity</s0>
<s5>20</s5>
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<fC03 i1="19" i2="2" l="SPA"><s0>Viscosidad</s0>
<s5>20</s5>
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<fC03 i1="20" i2="2" l="FRE"><s0>Epaisseur</s0>
<s5>21</s5>
</fC03>
<fC03 i1="20" i2="2" l="ENG"><s0>thickness</s0>
<s5>21</s5>
</fC03>
<fC03 i1="20" i2="2" l="SPA"><s0>Espesor</s0>
<s5>21</s5>
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<fC03 i1="21" i2="2" l="FRE"><s0>Cratère</s0>
<s5>22</s5>
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<fC03 i1="21" i2="2" l="ENG"><s0>craters</s0>
<s5>22</s5>
</fC03>
<fC03 i1="21" i2="2" l="SPA"><s0>Cráter</s0>
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<server><NO>PASCAL 13-0353144 INIST</NO>
<ET>The origin of graben and ridges in Rachmaninoff, Raditladi, and Mozart basins, Mercury</ET>
<AU>BLAIR (David M.); FREED (Andrew M.); BYRNE (Paul K.); KLIMCZAK (Christian); PROCKTER (Louise M.); ERNST (Carolyn M.); SOLOMON (Sean C.); MELOSH (H. Jay); ZUBER (Maria T.)</AU>
<AF>Department of Earth, Atmospheric, and Planetary Sciences, Purdue University/West Lafayette, Indiana/Etats-Unis (1 aut., 2 aut., 8 aut.); Department of Terrestrial Magnetism, Carnegie Institution of Washington, NW/Washington, DC/Etats-Unis (3 aut., 4 aut., 7 aut.); The Johns Hopkins University Applied Physics Laboratory/Laurel, Maryland/Etats-Unis (5 aut., 6 aut.); Lamont-Doherty Earth Observatory, Columbia University/Palisades, New York/Etats-Unis (7 aut.); Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology/Cambridge, Massachusetts/Etats-Unis (9 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Journal of geophysical research. Planets; ISSN 2169-9097; Etats-Unis; Da. 2013; Vol. 118; No. 1; Pp. 47-58; Bibl. 1 p.1/4</SO>
<LA>Anglais</LA>
<EA>The Rachmaninoff, Raditladi, and Mozart peak-ring impact basins on Mercury display a distinctive pattern of tectonic features consisting of a central zone that is either devoid of tectonic landforms or contains small ridges, a medial annulus of prominent and predominantly circumferentially oriented graben, and a distal zone displaying graben that occur in a mix of orientations and that are less evident toward the peak ring. Here we use finite element models to explore three candidate scenarios for the formation of these tectonic features: (1) thermal contraction of the interior smooth plains, (2) isostatic uplift of the basin floor, and (3) subsidence following volcanic loading. Our results suggest that only thermal contraction can account for the observed pattern of graben, whereas some combination of subsidence and global contraction is the most likely explanation for the central ridges in Rachmaninoff and Mozart. Thermal contraction models, however, predict the formation of graben in the centermost region of each basin, where no graben are observed. We hypothesize that graben in this region were buried by a thin, late-stage flow of plains material, and images of partially filled graben provide evidence of such late-stage plains emplacement. These results suggest that the smooth plains units in these three basins are volcanic in origin. The thermal contraction models also imply a cooling unit ∼1 km thick near the basin center, further supporting the view that plains-forming lavas on Mercury were often of sufficiently high volume and low viscosity to pool to substantial thicknesses within basins and craters.</EA>
<CC>001E01; 220</CC>
<FD>Graben; Mercure; Tectonique; Forme relief; Orientation; Méthode élément fini; Modèle; Contraction; Plaine; Surrection; Bassin subsidence; Subsidence; Monde; Ecoulement; Matériau; Mise en place; Refroidissement; Lave; Viscosité; Epaisseur; Cratère</FD>
<ED>grabens; mercury; tectonics; landforms; orientation; finite element analysis; models; contraction; plains; uplifts; subsidence basins; subsidence; global; flow; materials; emplacement; cooling; lava; viscosity; thickness; craters</ED>
<SD>Graben; Mercurio; Tectónico; Orientación; Modelo; Contracción; Llano; Cuenca de subsidencia; Subsidencia; Mundo; Emplazamiento; Enfriamiento; Lava; Viscosidad; Espesor; Cráter</SD>
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The origin of graben and ridges in Rachmaninoff, Raditladi, and Mozart basins, Mercury

The origin of graben and ridges in Rachmaninoff, Raditladi, and Mozart basins, Mercury

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