Parameter Amount Units Ref UMars Initial -5.23E+30 J F20 UMars Current -5.15E+30 J F20 ∆UExpansion = UMC – UMI 7.97E+28 J Result Table 3 - Potential Energy Difference Parameter Amount Units Ref RMars Current/RMars Initial 1.0202 m/m B7,F6 AMars Current/AMars Initial = (RMC/RMI) 2 1.0407 m2/m2 F28 VMars Current/VMars Initial = (RMC/RMI) 3 1.0617 m3/m3 F28 Sum of Crack Widths = 2π(RMC – RMI) 421 km Result Sum of Crack Areas = 4π(RMC 2 – RMI 2) 5,646,972 km2 Result Table 4 - Martian Thermal Expansion Ratios subtracting the small amount needed to provide expansion against gravity. Unlike the parallel set of calculations for the Earth, there is excess energy to heat Mars up to its currently estimated mantle temperature of 1280-1600°C (5). There is thus a need to account for the excess heat available via various loss channels, such as radiation, loss of water vapour and partial melting of Martian mantle material. A similar calculation has been undertaken for the Moon (17), where the heat loss channels itemised here were identified. The excess on both Mars was not as severe as that on the Moon. Nevertheless, during accelerated decay, radionuclides could have been concentrated in the eventual crustal material, selectively heating it to its boiling point (Table 4) before delivering it to the surface, from which radiative heat transfer (Table 6) can be estimated. It is not essential for the whole Martian surface to be molten, as the vigorous volcanic processes produced by accelerated decay would atomise the hot lava into fine droplets, which would have increased the effective surface area dramatically. The initial breakthrough of lava would have been through deep vertical channels near weak points in the planetary surface and would have happened at a catastrophic rate, creating mountains as high as the current crustal thickness. The boiling point of crustal lava has been estimated from that for SiO2 and the melting point for Mg2SiO4, the chief constituent of the mantle. The ratio of boiling to melting point has been assumed to be the same for both minerals, as this is true of the high-melting metals considered in Table 4. The prospect of heating minerals to their boiling points opens the door to evaporative heat loss, here estimated in Table 10, after that due to sensible heating of the mantle (Table 7), boiling of water (Table 8) and partial melting of the mantle (Table 9). The estimate for initial heating of the eventual crustal material (Table 5) is not included in the proposed heat balance (Table 11), as its heat would eventually find a place somewhere within the sinks indentified in Tables 6 to 10. References for input data are highlighted in yellow, with cited sources in the References table. If data is taken from another cell in the same sheet, the cell reference is shown, highlighted in cyan. If it is from another sheet, the sheet number appears before the cell reference. Along with key results, a magenta highlight indicates achievement of the goal of an initially ambient temperature before thermal expansion, using trial values of initial Martian radii. A time of order that of the Flood year, which would be isolated from observations of Martian surface disturbance, has been estimated for high-temperature radiative heat transfer from the planet. This also applies to the Moon. STERNBERG Craters and cracks 2023 ICC 57
RkJQdWJsaXNoZXIy MTM4ODY=