Geological evolution of Venus: Rises, plains, plumes, and plateaus

Science

Volumn 279, Issue 5356, 1998, Pages 1492-1497

  Phillips, Roger J ^a   Hansen, Vicki L ^b  

^a WASHINGTON UNIVERSITY   (United States)

^b SOUTHERN METHODIST UNIVERSITY   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

MANTLE PLUME; PLATEAU FORMATION; TECTONICS;

ASTRONOMY; EVOLUTION; GEOGRAPHY; GEOLOGY; GLOBAL CLIMATE; HISTORY; PRIORITY JOURNAL; REVIEW; VOLCANO;

VENUS;

EID: 0032489572     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.279.5356.1492     Document Type: Review

References (73)

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56. β. The value of β is different for thin-lid and thick-lid convection (and α ≡ 0 for thin-lid convection). Two coupled ordinary differential equations are integrated in time to obtain upper mantle (at base of lithospheric thermal boundary layer) and outermost core temperatures. Core energy balance includes the effects of solid inner core formation. Heat sources in the mantle are fractionated into a crust with time, and the heat flux out of the convecting mantle depends linearly on Nu.
57. The boundary layer bottom temperature is the outermost core temperature, and the top temperature is obtained by adiabatic extrapolation of the upper mantle solution temperature.
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60. The heat flow estimate in Table 1 is obtained from flexural modeling of a volcanic rise with a correction to the background value [R. J. Phillips et al., in (2), pp. 1163-1204].
61. -1, β (thin lid) = 0.33, and β (thick lid) = 0.30.
62. If these calculations are carried forward in time, partial melting reaches a peak and then starts to slowly decrease due to the loss of heat-producing radiogenic parent isotopes in the mantle. This is also the reason for the slope prior to the switch.
63. 2, 1 km average height above its surroundings) using an isostatic assumption. This yields the number of Tellus-sized crustal plateaus generated by plumes over the interval τ.
64. -2 during the interval 1.7 Ga to 0.7 Ga.
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68. This result is obtained by constructing a yield strength envelope [W. F. Brace and D. L. Kohlstedt, J. Geophys. Res. 85, 6248 (1980) ] using a dry diabase flow law [S. J. Mackwell, M. E. Zimmerman, D. L. Kohlstedt, D. S. Scherber, in Proc. of the 35th U.S. Symposium on Rock Mechanics, J. J. K. Daemen and R. A. Shultz, Eds. (A. A. Balkema, Rotterdam, 1995), pp. 207-214] and 10% strain in 0.1 My. The temperature profile used was for a cooling half-space model with a surface temperature of 740 or 1000 K and an initial temperature determined by mixing melt temperatures from the CMM with crustal temperatures from the CTM calculated with the appropriate surface temperature.
69. This result is obtained by constructing a yield strength envelope [W. F. Brace and D. L. Kohlstedt, J. Geophys. Res. 85, 6248 (1980) ] using a dry diabase flow law [S. J. Mackwell, M. E. Zimmerman, D. L. Kohlstedt, D. S. Scherber, in Proc. of the 35th U.S. Symposium on Rock Mechanics, J. J. K. Daemen and R. A. Shultz, Eds. (A. A. Balkema, Rotterdam, 1995), pp. 207-214] and 10% strain in 0.1 My. The temperature profile used was for a cooling half-space model with a surface temperature of 740 or 1000 K and an initial temperature determined by mixing melt temperatures from the CMM with crustal temperatures from the CTM calculated with the appropriate surface temperature.
70. J. C. Jaeger and N. G. W. Cook, Fundamentals of Rock Mechanics (Chapman & Hall, New York, 1979). The transition depth for tensile to shear failure is dependent on the choice of tensile yield stress. We used a value of 10 MPa, which is within the range estimated for intact basalts [R. A. Schultz, J. Geophys. Res. 95, 10883 (1993)].
71. J. C. Jaeger and N. G. W. Cook, Fundamentals of Rock Mechanics (Chapman & Hall, New York, 1979). The transition depth for tensile to shear failure is dependent on the choice of tensile yield stress. We used a value of 10 MPa, which is within the range estimated for intact basalts [R. A. Schultz, J. Geophys. Res. 95, 10883 (1993)].
72. C. G. Farnetani and M. A. Richards, J. Geophys. Res. 99, 13813 (1994).
73. This work was supported by NASA's Planetary Geology and Geophysics programs under Grants NAGW-3024 to Washington University and NAGW-2915 to Southern Methodist University. D. Brown and S. Hauck provided helpful reviews of earlier drafts of this manuscript. We thank M. Zuber and two additional reviewers for comments. J. Goodge provided a review of the revised manuscript.