4. Results: Dusty Case   b. Diurnal Changes of Horizontal Mean Fields up previous next
4.b.iii. Atmospheric heating profile

Figure 12d shows the horizontal and temporal mean vertical profiles of the atmospheric heating rate for potential temperature on day 6 of the dusty case. The major component of radiative heating above 2 km during daytime is dust absorption of solar radiation. The magnitude of convective heating and the depth of a convective cooling layer near the surface are similar to those of the dust-free case. During nighttime, the entire region of the calculated domain is subject to infrared radiative cooling due to CO2 and dust.

Each component of the radiative heating profile shown in Figure 12d is presented in Figure 12e. The profile of near infrared radiative heating due to CO2 is vertically uniform over the calculated domain. In the convective layer, where dust mixing ratio is uniform, the profile of radiative heating due to dust is vertically uniform. These two components tend to suppress thermal convection, since they warm the convection layer uniformly in the vertical direction. The radiative component that provides the largest contribution to driving thermal convection is the infrared heating due to CO2, which has a vertical profile concentrated near the surface.

Figure 12d: Diurnal change of horizontal and temporal mean vertical profiles of atmospheric heating rate (K/day) for potential temperature for day 6 of the dusty case. Orange line denotes convective heating, red line denotes infrared radiative heating, blue line denotes solar radiative heating, green line denotes turbulent diffusion of potential temperature, and the light purple line denotes heating due to turbulent dissipation. The lower panel shows a magnified view of the profiles below 1 km. Figure 12e: Diurnal change of horizontal and temporal mean vertical profiles of radiative heating rate (K/day) for day 6 of the dusty case. Red and purple lines denote infrared radiative heating due to CO2 and dust, respectively. Blue and light blue lines denote solar radiative heating due to CO2 and dust, respectively. The lower panel shows a magnified view of the profiles below 1 km.


A numerical simulation of thermal convection in the Martian lower atmosphere with a two-dimensional anelastic model
Odaka, Nakajima, Ishiwatari, Hayashi,   Nagare Multimedia 2001
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