類地行星熱物理?xiàng)l件與熱演化影響因素分析——以火星地幔熱柱演化為例
[Abstract]:Earth-like planets in the solar system have a similar lithospheric ring structure surrounding the core of the metal, and are of simultaneous and homology in the historical origin of the thermal evolution of the planetary mantle. Both of them are cooled with the decay of radioactive heat energy on the basis of early deformation gravity potential energy heating. However, its thermal evolution history has its own characteristics due to the difference of physical conditions such as radius, density, viscosity and surface tectonic properties. Based on the basic thermal convection and heat conduction equations, we calculate and analyze the influence of the difference of geo-planetary thermo-physical conditions on the thermal evolution history of the planetary mantle. The results show that the thermal convection of the mantle is the main heat dissipation mode in the early stage of the thermal evolution of the terrestrial planets. The larger radius of the planet surface heat flux, the average heat loss is also large. The inner temperature difference of the planet with small radius is small, the viscosity coefficient is high, the convection ability is low, the planet enters the heat conduction state early, and the lithosphere with the conduction heat dissipation is thicker than the big planet. Under different boundary layer thermophysical conditions, the thermal evolution history of planetary like mantle will be gradually cooled, which includes the fluctuation of upwelling heat plume and the periodic mode of planetary mantle curtain subturnover. The mantle thermal plume in Mars is closely related to the thermal evolution of the Martian mantle. Based on the Martian mantle thermodynamics evolution model, the characteristics of mantle thermal dynamics evolution related to mantle thermal plume tectonic evolution are quantitatively calculated, and the three-dimensional spherical crust numerical simulation is carried out. The nonmonotonic variation of the thermal evolution history of Mars caused by the possible thermal plume activity in the Martian mantle and the evolution of the convective ring structure of the mantle over time are studied. And the influence of the mantle plume related to the boundary on the topography of Mars.
【作者單位】: 中國科學(xué)院大學(xué)中國科學(xué)院計(jì)算地球動(dòng)力學(xué)重點(diǎn)實(shí)驗(yàn)室;
【基金】:國家自然科學(xué)基金項(xiàng)目(編號(hào):41174085) 中國科學(xué)院創(chuàng)新團(tuán)隊(duì)項(xiàng)目(編號(hào):KZZD-EW-TZ-19) 中國科學(xué)院戰(zhàn)略性先導(dǎo)科技專項(xiàng)(編號(hào):XDA1103010102)資助
【分類號(hào)】:P185.3
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