Heat deposition and retention in a solid planet growing by impacts

Details Heat deposition and retention in a solid planet growing by impacts Heat deposition and retention in a solid planet growing by impacts

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icar...63...45d&link_type=abstract

Icarus (ISSN 0019-1035), vol. 63, July 1985, p. 45-68.

Astronomy and Astrophysics

Astronomy

24

Astronomical Models, Impact Damage, Kinetic Heating, Planetary Evolution, Planetary Temperature, Solid Phases, Advection, Conductive Heat Transfer, Cratering, Scaling Laws, Temperature Distribution, Terrestrial Planets, Thermal Diffusivity, Vertical Distribution, Planets, Heat, Deposition, Impacts, Parameters, Size, Velocity, Radius, Formation, Scaling, Heating, Depth, Melting, Terrestrial Planets

Scientific paper

The scaling and impact effects and the resulting heat deposition and retention by a young, growing planet accreting material before the stage of significant solid- or liquid-convection are examined analytically. Attention is given to various conditions of heat conduction associated with vertical advection. The discussion yields three length parameters useful for examining impact heating by means of the Holsapple and Schmidt (1982) model. The theory is extended to a variety of impactor sizes to derive limiting values for the controlling parameters, i.e., penetration depth, heating and cooling rates, to predict the efficiency of heat retention. It is predicted that a terrestrial-sized planet will retain sufficient heat to experience melting at a 2000-3000 km radius. The uncertainties in the calculations could be as much as a factor of two.

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