Geoid and topography of Venus in various thermal convection models

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F12%3A10123805" target="_blank" >RIV/00216208:11320/12:10123805 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1007/s11200-011-0251-7" target="_blank" >http://dx.doi.org/10.1007/s11200-011-0251-7</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1007/s11200-011-0251-7" target="_blank" >10.1007/s11200-011-0251-7</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Geoid and topography of Venus in various thermal convection models

Popis výsledku v původním jazyce

Important though indirect information about the internal structure of Venus is provided by its topography and geoid. In the last decades this information has been used to constrain the Venus mantle viscosity structure and its dynamic regime. Recently, the geodynamic inversion of the Venus' geoid and topography resulted in a group of best fitting viscosity profiles. We use these viscosity models here as an input to our mantle convection code. We carry out simulations of the Venus' mantle evolution in a 3D spherical shell with depth dependent viscosity and check whether the character of the dynamic topography and the geoid represented by their power spectra fits the observed quantities. We compare the results with several other models obtained for different viscosity stratifications (constant, constant with highly viscous lithosphere, linear increase of viscosity). Further, we estimate the effect of other factors such as internal heating and varying Rayleigh number. We use a 2D spherical

Název v anglickém jazyce

Geoid and topography of Venus in various thermal convection models

Popis výsledku anglicky

Important though indirect information about the internal structure of Venus is provided by its topography and geoid. In the last decades this information has been used to constrain the Venus mantle viscosity structure and its dynamic regime. Recently, the geodynamic inversion of the Venus' geoid and topography resulted in a group of best fitting viscosity profiles. We use these viscosity models here as an input to our mantle convection code. We carry out simulations of the Venus' mantle evolution in a 3D spherical shell with depth dependent viscosity and check whether the character of the dynamic topography and the geoid represented by their power spectra fits the observed quantities. We compare the results with several other models obtained for different viscosity stratifications (constant, constant with highly viscous lithosphere, linear increase of viscosity). Further, we estimate the effect of other factors such as internal heating and varying Rayleigh number. We use a 2D spherical

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

DE - Zemský magnetismus, geodesie, geografie

OECD FORD obor

—

Projekt

—

Návaznosti

Z - Vyzkumny zamer (s odkazem do CEZ)<br>S - Specificky vyzkum na vysokych skolach

Rok uplatnění

2012

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

STUDIA GEOPHYSICA ET GEODAETICA

ISSN

0039-3169

e-ISSN

—

Svazek periodika

56

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

CZ - Česká republika

Počet stran výsledku

19

Strana od-do

621-639

Kód UT WoS článku

000305218200017

EID výsledku v databázi Scopus

—