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Scaling of temperature- and pressure-dependent viscosity convection

Hüttig, C. und Breuer, D. (2008) Scaling of temperature- and pressure-dependent viscosity convection. In: EPSC Abstracts, 3, Seite 455. 3rd European Planetary Science Congress, 2008-09-21 - 2008-09-26, Münster, Westfalen (Germany).

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Kurzfassung

<p>In a series of three-dimensional spherical simulations the effects of purely internally heated convection was studied to yield updated scaling laws for parameterized mantle convection models similar to 2D boxed approaches as [1], [2]. The upper Rayleigh number, the viscosity contrast due to temperature and pressure were varied in over 88 cases to study the influence of these parameters on the quasi steady-state. A viscosity contrast up to the order of 10<sup>9</sup> was observed. The simulations were carried out using the new GAIA framework, consisting of a highly parallel solver for mantle convection in arbitrary geometries. Updated values for the Nusselt – Rayleigh scaling are presented together with a new mobility criterion to specify the stagnant lid regime. Furthermore, the parametric ranges of degree-one convection are presented along with a new spectral scaling that allows the determination of the internal Rayleigh number from dominant spherical harmonic modes of convective systems. If the viscosity contrast within the system reaches a certain limit, the style changes to stagnant lid convection. In the regime of stagnant lid convection, the dominant mode increases if the internal Rayleigh number is increased as well, while in the non-stagnant lid regime the modes stay low (bifurcation), as shown in figure 1.</p><p> Comparing the results to those previously published ([1], [2], [3], [4]) in the same parameter range in 2D and 3D boxes exposed an interesting increase of the γ parameter relating the transition to the stagnant lid regime. It seems that 2D or 3D boxed runs produce a stagnant lid while in a sphere fall into degree-one convection without a stagnant lid. A transitional or sluggish regime could not be observe d. The viscosity contrast at which stagnant lid convection occurs could be pin-pointed to 2.96e4 with a confidence interval of less than +/-2.7e3. Spectral analysis revealed also that stagnant lid convection cannot happen below a degree four pattern and that degree-one convection is not possible for iso-viscous convection because the range in which degree-one convection would occur leads to a Rayleigh number not high enough to enable convection.</p><p> The newly derived spectral scaling law was applied to gravity field observations of Venus to constrain and compare internal parameters such as viscosity and temperature at the convecting interior with previously published values.</p> [1] Solomatov, V.S. and Moresi, L.-N. (2000) JGR, 105, p.21,795-21,817.<br /> [2] Grasset, O. and Parmentier, E.M. (1998) JGR, 103, p18,171-18,181 <br /> [3] Dumoulin, C., Doin, M.-P. and Fleitout, L. (1999) JGR, 104, p.12,759-12,777.<br /> [4] Reese, C.C., Solomatov, V.S., Baumgardner, J.R., Yang, W.-S. (1999) PEPI, 116, p1-7.

Dokumentart:Konferenzbeitrag (Vortrag)
Titel:Scaling of temperature- and pressure-dependent viscosity convection
Autoren:
AutorenInstitution oder E-Mail-Adresse der Autoren
Hüttig, C.NICHT SPEZIFIZIERT
Breuer, D.NICHT SPEZIFIZIERT
Datum:22 September 2008
Erschienen in:EPSC Abstracts
Referierte Publikation:Nein
In SCOPUS:Nein
In ISI Web of Science:Nein
Band:3
Seitenbereich:Seite 455
Status:veröffentlicht
Stichwörter:convection, 3D sperical simulations, GAIA framework, Nusselt-Rayleigh scaling, stagnant lid, Venus
Veranstaltungstitel:3rd European Planetary Science Congress
Veranstaltungsort:Münster, Westfalen (Germany)
Veranstaltungsart:internationale Konferenz
Veranstaltungsdatum:2008-09-21 - 2008-09-26
HGF - Forschungsbereich:Verkehr und Weltraum (alt)
HGF - Programm:Weltraum (alt)
HGF - Programmthema:W EW - Erforschung des Weltraums
DLR - Schwerpunkt:Weltraum
DLR - Forschungsgebiet:W EW - Erforschung des Weltraums
DLR - Teilgebiet (Projekt, Vorhaben):W - Vorhaben Vergleichende Planetologie (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung > Planetenphysik
Hinterlegt von: Stefanie Hempel
Hinterlegt am:17 Okt 2008
Letzte Änderung:27 Apr 2009 15:15

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