Differences of Venus from Earth Attributable to Origin Circumstances

Details Differences of Venus from Earth Attributable to Origin Circumstances Differences of Venus from Earth Attributable to Origin Circumstances

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998lpico.957...27n&link_type=abstract

Origin of the Earth and Moon, Proceedings of the Conference held 1-3 December, 1998 in Monterey, California. LPI Contribution N

Physics

Rare Gases, Solar System, Venus (Planet), Earth (Planet), Asteroid Collisions, Simulation, Magnetic Fields, Argon, Krypton, Hypervelocity Impact

Scientific paper

Most of the marked differences in Venus from Earth can be attributed to evolutionary circumstances, particularly those arising from a deficiency of water in Venus' outer layers. But three major differences depend on circumstances of origin: (1) the absence of a magnetic field; (2) the retrograde spin and, thence, no satellite; and (3) the greater abundance of primordial inert gases. The absence of a magnetic field is apparently due to Venus being sufficiently smaller than Earth; as a result, it does not have a solidifying inner core as the energy source for a dynamo. The close to 180 degree retrograde spin plausibly arose from an initial retrograde spin of higher obliquity [2], as well as the driving of the spin to a Cassini state by dissipation. The excesses of Venus over Earth by a factor of 4 or so of Xe and Kr plausibly arose from the Earth receiving by far the larger impact during accretion. But the much larger excesses of Ne and Ar suggest a unique event: the impact into Venus of an icy large body from far out in the solar system. Until recently, this hypothesis was thought to be physically unfeasible because of the near-impossibility of reducing approach velocities appreciably. This discussion will focus on new developments in large impact simulation that change this perception.

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