Photoevaporation of the solar nebula and the formation of the giant planets

Details Photoevaporation of the solar nebula and the formation of the giant planets Photoevaporation of the solar nebula and the formation of the giant planets

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993icar..106...92s&link_type=abstract

Icarus, vol. 106, p. 92

Computer Science

102

Solar Corona, Evaporation, Planetary Evolution, Jupiter (Planet), Stellar Winds, T Tauri Stars, Saturn (Planet), Neptune (Planet)

Scientific paper

In order to account for the observed differences in envelope mass relative to core mass between the gas-rich and gas-poor giant planets, a discriminant is proposed that relies on the effect of photoevaporation by Lyman continuum photons of the outer portions of the disk as the primary mechanism of hydrogen and helium loss. The orbit of Saturn is noted to constitute the natural transitional radius between gas retention and loss. The evaporative wind of the Saturn-Neptune regions would have sufficed to purge H and He gas prior to the planets' reaching a critical core mass for runaway gas accretion, is the primitive sun possessed enhanced EUV luminosity over a period comparable to that of T Tauri stars.

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