Impact jetting of water ice, with application to the accretion of icy planetesimals and Pluto

Details Impact jetting of water ice, with application to the accretion of icy planetesimals and Pluto Impact jetting of water ice, with application to the accretion of icy planetesimals and Pluto

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989georl..16.1237m&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 16, Nov. 1989, p. 1237-1240.

Physics

11

Hydraulic Jets, Icy Satellites, Pluto (Planet), Protoplanets, Solar Corona, Carbon Monoxide, Charon, Hugoniot Equation Of State, Impact Melts

Scientific paper

Jetting can occur during oblique impacts of water-ice bodies at relative velocities as low as 500 m/sec, because of the low Hugoniot elastic limit and high compressibility of ice compared to rock. In jetted ice, incipient melting, complete melting, and incipient vaporization occur, upon release to low pressure, at impact velocities of 1.3, 2.0, and 2.7 km/sec, respectively, much less than the 3.4, 4.4, and 5.3 km/sec, required in head-on collisions. Uncertainties in the shock equation-of-state may allow complete melting during jetting of relative velocities as low as 1.2 km/sec. Because jet speeds exceed impact speeds during the accretion of icy bodies greater than a few 100 km in radius, there may be a significant loss of icy material. Thus, jetting during a Charon-forming collision (and not vaporization) may account for Pluto-Charon's relatively large rock/ice ratio, should the C/O ratio of the solar nebula turn out to be too low to sufficiently raise the rock/ice ratio of outer solar nebula condensates by formation of noncondensable CO.

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