Midplane temperatures in the solar nebula

Details Midplane temperatures in the solar nebula Midplane temperatures in the solar nebula

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993lpi....24..151b&link_type=abstract

In Lunar and Planetary Inst., Twenty-fourth Lunar and Planetary Science Conference. Part 1: A-F p 151-152 (SEE N94-12015 01-91)

Astronomy and Astrophysics

Astronomy

Accretion Disks, Cosmochemistry, Meteoritic Composition, Nebulae, Planetary Nebulae, Solar System Evolution, Astronomical Models, Contraction, Heating, Hydrodynamics, Protostars, Stellar Mass, Sun

Scientific paper

Cosmochemical analyses of meteorites imply that maximum temperatures in the inner solar nebula were on the order of 1300 K, yet standard viscous accretion disk models predict much lower midplane temperatures (approx. 300 K at 2 AU to 3 AU) in a minimum mass nebula. A second-order accurate radiative hydrodynamics code has been used to construct models of the late-phase solar nebula appropriate for low-mass star formation (M is approximately 10-6 to 10-5 solar-M yr-1. For a minimum mass (0.02 solar-M) nebula and a solar-mass protostar, the new models show that compressional heating due to mass accretion onto the nebula and subsequent vertical contraction of the nebula are sufficient to lead to midplane temperatures Tm greater than 1400 K at 1 AU and Tm greater than 1000 K at 2.5 AU.

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