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A.d.i. Radiative transfer of atmospheric CO2
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Both infrared and near infrared radiative fluxes associated with
CO2 are calculated by using the Goody narrow band model
(cf., Goody and Young, 1989).
By using this band model, the temperature profile from 10 to 15 km,
which is corresponds to the tropopause region of the dust-free
Martian atmosphere, can be calculated precisely.
In calculating the infrared radiative flux, only the CO2 15
μm band is taken into consideration.
The upward and downward infrared radiative fluxes
( ) and the infrared radiative heating rate
per unit mass  are calculated as follows.
 is the i th narrow band width and
 is the Plank function which is represented as follows.
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(A.26) |
where  is the Plank constant,
 is the speed of light,
 is the Boltzmann constant,
 is temperature.
 is the transmission function averaged over
for  .
 is line strength,
 is the square root of the product of line
strength and line width,
 is the reference value of
,
 is effective path length, and
 is the reference pressure (1013 hPa).
When calculating the near infrared solar radiative flux, the
CO2 4.3 μm, 2.7 μm, and 2.0 μm bands are
considered.
The near infrared solar radiative flux  and the near
infrared radiative heating rate per unit mass 
are calculated as follows.
where  ,
 is the solar zenith angle,
 is the solar radiative flux at the top
of the atmosphere, which is represented as follows.
where  is the surface temperature of the sun (5760 K),
 is the Stefan-Boltzmann constant
(5.67×10-8 Wm-2K-4),
 is the solar constant at the mean radius of Mars' orbit
(591 Wm-2),
 and
 are the radius of Mars' orbit and its mean value,
 is the solar radiative flux integrated over all wavelength
at the top of the atmosphere.
varies with season, latitude and local time.
Detail descriptions of
and
 are shown in Appendix A.d.vi.
The transmission function averaged over in the near
infrared wavelength region is similar to that in the infrared
wavelength region, except for the effective path length
.
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