Ortho-para-hydrogen equilibration on Jupiter

Details Ortho-para-hydrogen equilibration on Jupiter Ortho-para-hydrogen equilibration on Jupiter

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...393..357c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 393, no. 1, July 1, 1992, p. 357-372. Research supported by NASA.

Astronomy and Astrophysics

Astrophysics

13

Iris Satellites, Jupiter Atmosphere, Ortho Hydrogen, Para Hydrogen, Thermodynamic Equilibrium, Voyager Project, Ammonia, Infrared Interferometers, Jupiter (Planet), Radiative Transfer

Scientific paper

Voyager IRIS observations reveal that the Jovian para-hydrogen fraction is not in thermodynamic equilibrium near the NH3 cloud top, implying that a vertical gradient exists between the high-temperature equilibrium value of 0.25 at depth and the cloud top values. The height-dependent para-hydrogen profile is obtained using an anisotropic multiple-scattering radiative transfer model. A vertical correlation is found to exist between the location of the para-hydrogen gradient and the NH3 cloud, strongly suggesting that paramagnetic conversion on NH3 cloud particle surfaces is the dominant equilibration mechanism. Below the NH3 cloud layer, the para fraction is constant with depth and equal to the high-temperature equilibrium value of 0.25. The degree of cloud-top equilibration appears to depend on the optical depth of the NH3 cloud layer. Belt-zone variations in the para-hydrogen profile seem to be due to differences in the strength of the vertical mixing.

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