"I accept that there is a great deal of kinetic energy to be converted
to heat. As I explained before, this heat can be dissipated in many different ways including the fragmentation of solid material and melting of this to form metamorphic rocks. Plenty of evidence of this everywhere-no need to do a calculation starting from uncertain assumptions as to size density and initial temperatures etc of the affected zones. "
--The impact of the projectile sends shock waves traveling into both bodies. By the time that the shock waves have reached the back surface of the projectile the energy of the system is in four forms:
[1] - kinetic energy of the projectile which is still moving;
[2] - internal energy of the projectile mostly in the form of shock compression;
[3] - kinetic energy of the target material; and
[4] - internal energy of target material, again mostly as shock compression.
--When the shock wave has reached the end of the projectile a rarefaction wave travels backwards restoring some kinetic energy but also producing heat. Material is ejected, initially at low angles to the surface of the target but at speeds up to three times that of the projectile. Material ejected at a later time is a greater angles to the surface but travels more slowly.
The final destination of the energy originally in the projectile is approximately--heat 31%, ejected material 49% and crushing(producing surface energy) 19% with the small residue going into spallation.
--It is not at all certain how to extrapolate these results into the regime of a planetary collision in which there are many additional features:
[1] - For bodies of comparable size there is no distinction between projectile and target.
[2] - The impact velocities and hence the shock compressions will be much higher than in any laboratory experiment.[3] - The ejecta may be massive and their dispersion greatly influenced by gravitational forces.
[4] - Gravitational energy will be important for planetary bodies, especially in influencing their approach speeds.
[Woolfson, 2000 - The origin and evolution of the solar system]
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