Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007georl..3424201m&link_type=abstract
Geophysical Research Letters, Volume 34, Issue 24, CiteID L24201
Physics
16
Planetary Sciences: Comets And Small Bodies: Impact Phenomena (5420, 8136), Planetary Sciences: Solid Surface Planets: Ices, Planetary Sciences: Solid Surface Planets: Origin And Evolution, Tectonophysics: Heat Generation And Transport
Scientific paper
The thermal evolution of planets during their growth is strongly influenced by impact heating. The temperature increase after a collision is mostly located next to the shock. For Moon to Mars size planets where impact melting is limited, the long term thermo-mechanical readjustment is driven by spreading and cooling of the heated zone. To determine the time and length scales of the adjustment, we developed a numerical model in axisymmetric cylindrical geometry with variable viscosity. We show that if the impactor is larger than a critical size, the spherical heated zone isothermally flattens until its thickness reaches a value for which motionless thermal diffusion becomes more effective. The thickness at the end of advection depends only on the physical properties of the impacted body. The obtained timescales for the adjustment are comparable to the duration of planetary accretion and depend mostly on the physical properties of the impacted body.
Coltice Nicolas
Dubuffet Fabien
Monteux Julien
Ricard Yanick
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