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Atmospheric RadiationTheoretical Basis$
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R. M. Goody and Y. L. Yung

Print publication date: 1989

Print ISBN-13: 9780195051346

Published to Oxford Scholarship Online: November 2020

DOI: 10.1093/oso/9780195051346.001.0001

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Evolution of a Thermal Disturbance

Evolution of a Thermal Disturbance

(p.426) 10 Evolution of a Thermal Disturbance
Atmospheric Radiation

R. M. Goody

Y. L. Yung

Oxford University Press

The thermodynamic equation for an ideal gas is where ρcv6 is the internal energy per unit volume and hR is the radiative heating rate. For the sake of clarity we omit diabatic terms additional to the radiative heating. We may expand the left-hand side of (10.1) and write it in the form of an enthalpy equation, and cp is the specific heat at constant pressure. The left-hand side of includes both internal and potential energy, d is the dynamic heating. If the vertical coordinate is pressure, ∂p/∂t = 0 and all terms in d tend to zero as the velocities tend to zero. Solutions to (10.2) in conjunction with the equations of motion, the equation of continuity, and the gas law are the matter of dynamic meteorology. In this chapter, we look at a single aspect, namely the coupling between radiation and dynamics as expressed by the thermodynamic equation, (10.2). We shall use the methods of perturbation theory. Assume the existence of a basic, steady-state (suffix 0) for which This basic state could be a state of radiative equilibrium or a state dominated by dynamic transports.

Keywords:   Adiabatic lapse rate, Boundary exchange, Diabatic heating, Diffusivity factor, Emission temperature, Grey absorption, Internal energy, Logarithmic regime, Mercury, Newtonian cooling

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