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Investigation of Venus’ Thermal History, Crustal Evolution, and Core Dynamics with a Coupled Interior-lithosphere-atmosphere Model

  • Authors: Rodolfo Garcia, Rory Barnes, Peter E. Driscoll, Victoria S. Meadows, Megan Gialluca

Rodolfo Garcia et al 2026 The Planetary Science Journal 7 .

  • Provider: AAS Journals

Caption: Figure 21.

The evolution of the different factors in the core temperature evolution (Equation 5). The top panel shows the amount of cooling due to convective loss to the mantle (QCMB), the second panel shows the amount of heating due to decay of radioactive elements (﹩{Q}_{i,{\rm{core}}}﹩), the third panel shows the sum of core heating/cooling effects (latent, gravitational, and compositional energy), and the bottom panel shows the scaling factor due to the size of the inner core and its influence on secular cooling, i.e., the denominator in Equation (5). Note that Type III evolutions (red) have a higher scaling factor and, thus, will cool or heat less from the same amount of energy as non–Type III evolutions.

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