Net radiative heating in the middle atmosphere |
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| Institution: | 1. Unidad Académica de Física, Universidad Autónoma de Zacatecas, Calzada Solidaridad Esquina Paseo a la Bufa s/n, CP 98060, Mexico;2. CONACYT-Instituto de Investigación en Comunicación Óptica, Universidad Autónoma de San Luis Potosí, Av. Karakorum 1470, Lomas 4a sección, San Luis Potosí, SLP 78210, Mexico;1. Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstr. 25/8, 6020, Innsbruck, Austria;2. Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos, 0610, Antofagasta, Chile;3. Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077, Göttingen, Germany;4. Department of Astrophysics, University of Vienna, Türkenschanzstr. 17, 1180, Vienna, Austria;5. Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, 85748, Garching, Germany;1. Department of Electrical Engineering, The Pennsylvania State University, University Park, PA, USA;2. Department of Physics, The Pennsylvania State University-Lehigh Valley, Center Valley, PA, USA;3. Department of Electrical Engineering, University of Illinois-Urbana Champaign, IL, USA |
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| Abstract: | The meridional distributions of both total solar and net radiative heating rates have been obtained between 30 and 110 km at both the solstice and equinox using Fomichev et al.'s total radiative long wave cooling data in the calculations of the net radiative heating. The contributions to the solar heating of O3, O2, CO2 and H2O have been investigated. For the ozone heating, the absorption of diffusive solar radiation from the ground and troposphere has been estimated. The 50–90 km layer is close to radiative equilibrium on a globally averaged basis. The importance of radiative cooling as an energy sink in the 90–110 km layer is apparently not less than that of the vertical eddy heat conduction. The ordered meridional circulation has been obtained under the assumption that the temperature variation, due to net radiative heating, is balanced by the adiabatic and temperature variations due to vertical air motion. The circulation model obtained is compared with other empirical models, which are reviewed. For the hemisphere and the 60–80 km layer, the two-cell circulation with the rising motion near the equator and pole from spring to autumn and above 80 km, the one-cell circulation with the sinking motion near the equator and equinox, seem to be most realistic. Also quite realistic for the period near the solstice is the same type of two-cell circulation in the 40–50 km layer and the sinking motion at low latitudes in the 50–60 km layer. |
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