With standard name-list settings, both the longwave and shortwave heating rates are evaluated every model hour. Between hourly evaluations, the longwave and shortwave fluxes and flux divergences are held constant.
In CAM 3.0, insolation is computed using the method of
Berger [17]. Using this formulation, the insolation can be
determined for any time within years of 1950 AD. This
facilitates using CAM 3.0 for paleoclimate simulations. The insolation
at the top of the model atmosphere is given by
We represent the annual and diurnal cycle of solar insolation with a repeatable solar year of exactly 365 days and with a mean solar day of exactly 24 hours, respectively. The repeatable solar year does not allow for leap years. The expressions defining the annual and diurnal variation of solar insolation are:
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(4.175) |
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(4.176) |
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(4.177) |
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(4.178) |
where
| ||
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|
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|
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|
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|
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(4.179) |
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|
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|
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|
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The hour angle in the expression for
depends on the
calendar day
as well as model longitude:
The obliquity may be approximated by an empirical series
expansion of solutions for the Earth's orbit
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(4.181) |
Since the series expansion for the eccentricity is slowly
convergent, it is computed using
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(4.182) |
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(4.183) |
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(4.184) |
The general precession is given by another empirical series expansion
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(4.185) |
The calculation of requires first determining two mean
longitudes for the orbit. The mean longitude
at the
time of the vernal equinox is :
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|
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(4.186) | ||
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(4.187) |
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|
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(4.188) | |
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The orbital state used to calculate the insolation is held fixed over
the length of the model integration. This state may be specified in
one of two ways. The first method is to specify a year for computing
. The value of the year is held constant for the entire length of
the integration. The year must fall within the range of
. The second method is to specify the eccentricity factor
,
longitude of perihelion
, and obliquity
. This set of values is sufficient to specify the complete
orbital state. Settings for AMIP II style integrations under 1995 AD
conditions are
,
, and
.
The solar spectrum is divided into 19 discrete spectral and
pseudo-spectral intervals (7 for
, 1 for the visible,
7 for
, 3 for
, and 1 for the
near-infrared following Collins [37]). The CAM 3.0 model
atmosphere consists of a discrete vertical set of horizontally
homogeneous layers within which radiative heating rates are to be
specified (see Figure 3.1). Each of these layers is
considered to be a homogeneous combination of several radiatively
active constituents. Solar irradiance, surface reflectivity for
direct and diffuse radiation in each spectral interval, and the cosine
of the solar zenith angle are specified. The surface albedo is
specified in two wavebands (0.2-0.7
m, and 0.7-5.0
m) and
distinguishes albedos for direct and diffuse incident radiation.
Albedos for ocean surfaces, geographically varying land surfaces, and
sea ice surfaces are distinguished.
The method involves evaluating the -Eddington solution for the
reflectivity and transmissivity for each layer in the vertical under
clear and overcast conditions. The layers are then combined together,
accounting for multiple scattering between layers, which allows
evaluation of upward and downward spectral fluxes at each interface
boundary between layers. This procedure is repeated for each spectral
or pseudo-spectral interval and binary cloud configuration (see
``Cloud vertical overlap'' below) to accumulate broad band fluxes,
from which the heating rate can be evaluated from flux differences
across each layer. The
-Eddington scheme is implemented so
that the solar radiation is evaluated once every model hour (in the
standard configuration) over the sunlit portions of the model earth.
The -Eddington approximation allows for gaseous absorption by
,
,
, and
. Molecular scattering and scattering/absorption by
cloud droplets and aerosols are included. With the exception of
, a summary of the spectral
intervals and the absorption/scattering data used in the formulation
are given in Briegleb [27] and Collins [37]. Diagnostic
cloud amount is evaluated every model hour just prior to the solar
radiation calculation.
The absorption by water vapor of sunlight between 1000 and 18000
cm is treated using seven pseudo-spectral intervals. A
constant specific extinction is specified for each interval. These
extinctions have been adjusted to minimize errors in heating rates and
flux divergences relative to line-by-line (LBL) calculations for
reference atmospheres [3] using GENLN3
[57] combined with the radiative transfer solver DISORT2
[163]. The coefficients and weights have the same
properties as a k-distribution method [98], but this
parameterization is essentially an exponential sum fit (e.g.,
Wiscombe and Evans [191]). LBL calculations are performed with the HITRAN2k line database
[153] and the Clough, Kneizys, and Davies (CKD)
model version 2.4.1 [33]. The Rayleigh scattering optical
depths in the seven pseudo-spectral intervals have been changed for
consistency with LBL calculations of the variation of water-vapor
absorption with wavelength. The updated parameterization
increases the absorption of solar radiation by water vapor relative
to the treatment used in CCM and CAM since its introduction by
Briegleb [27].
For some diagnostic purposes, such as estimating cloud radiative forcing [94] a clear-sky absorbed solar flux is required. In CAM 3.0, the clear-sky fluxes and heating rates are computed using the same vertical grid as the all-sky fluxes. This replaces the 2-layer diagnostic grid used in CCM3.
The treatment of aerosols in CAM 3.0 replaces the uniform background boundary-layer aerosol used in previous versions of CAM and CCM. The optics for the globally uniform aerosol were identical to the sulfate aerosols described by Kiehl and Briegleb [88]. In the visible, the uniform aerosol was essentially a conservative scatterer. The new treatment introduces five chemical species of aerosol, including sea salt, soil dust, black and organic carbonaceous aerosols, sulfate, and volcanic sulfuric acid. The new aerosols include two species, the soil dust and carbonaceous types, which are strongly absorbing in visible wavelengths and hence increase the shortwave diabatic heating of the atmosphere.
The three-dimensional time-dependent distributions of the five aerosol species and the optics for each species are loaded into CAM 3.0 during the initialization process. This provides considerable flexibility to:
In its present configuration, CAM includes the direct and semi-direct effects of tropospheric aerosols on shortwave fluxes and heating rates. The first indirect effect, or Twomey et al. [175] effect, is not included in the standard version of CAM 3.0.
The annually-cyclic tropospheric aerosol climatology consists of three-dimensional, monthly-mean distributions of aerosol mass for:
The climatology is produced using an aerosol assimilation system [39,41] integrated for present-day conditions. The system consists of the Model for Atmospheric Chemistry and Transport (MATCH) [142] and an assimilation of satellite retrievals of aerosol optical depth. MATCH version 4 is integrated using the National Centers for Environmental Prediction (NCEP) meteorological reanalysis at T63 triangular truncation [83]. The satellite estimates of aerosol optical depth are from the NOAA Pathfinder II data set [167].
The formulation of the sulfur cycle is described in Barth et al. [12]
and Rasch et al. [143]. The emissions inventory for SO is from
Smith et al. [162].
The sources for mineral dust are based upon
the approach of Zender et al. [196] and Mahowald et al. [120].
The emissions of carbonaceous aerosols include contributions from
biomass burning [113], fossil fuel burning
[42], and a source of
natural organic aerosols resulting from terpene emissions. The
vertical profiles of sea salt are computed from the 10m wind speed
[21].
The monthly-mean mass path for each aerosol species in each layer is
computed in units of kg/m. During the initialization of CAM 3.0,
the climatology is temporally interpolated from monthly-mean to mid-month
values. At each CAM 3.0 time step, the mid-month values bounding the
current time step are vertically interpolated onto the pressure grid
of CAM 3.0 and then time interpolated to the current time step. The
interpolation scheme in CAM 3.0 preserves the aerosol masses for each
species to 1 part in 10
relative to the climatology, and it is
guaranteed to yield positive definite mass-mixing ratios for all
aerosols.
The stratospheric volcanic aerosols are treated using a single species
in the standard model. Zonal variations in the stratospheric mass
loading are omitted. The volcanic input consists of the monthly-mean
masses in units of kg/m on an arbitrary meridional and vertical
grid. The time series for the recent past is based upon
Ammann et al. [2] following Stenchikov et al. [166].
The three intrinsic optical properties stored for each of the eleven aerosol types are specific extinction, single scattering albedo, and asymmetry parameter. These properties are computed on the band structure of CAM 3.0 using Chandrasekhar weighting with spectral solar insolation. The aerosol types affected by hygroscopic growth are sulfate, sea salt, and hydrophilic organic carbon. In previous versions of CCM and CAM 3.0, the relative humidity was held constant in calculations of hygroscopic growth at 80%. In CAM 3.0, the actual profiles of relative humidity computed from the model state each radiation time step are used in the calculation.
The optics for black and organic carbon are identical to the optics
for soot and water-soluble aerosols in the Optical Properties of
Aerosols and Clouds (OPAC) data set [69]. The optics for
dust are derived from Mie calculations for the size distribution
represented by each size bin [196]. The Mie
calculations for sulfate assume that it is comprised of ammonium
sulfate with a log-normal size distribution. The dry size parameters
are a median radius of 0.05 m and a geometric standard deviation
of 2.0. The optical properties in the seven H
O pseudo-spectral
intervals are averaged consistently with LBL calculations of the
variation of water-vapor absorption with wavelength. This averaging
technique preserves the cross correlations among the spectral
variation of solar insolation, water vapor absorption, and the aerosol
optical properties.
The volcanic stratospheric aerosols are assumed
to be comprised of 75% sulfuric acid and 25% water. The log-normal
size distribution has an effective radius of 0.426
m and a
standard deviation of 1.25.
The bulk formulae of Cess [30] are used to combine the optical properties of the individual aerosol species into a single set of bulk aerosol extinctions, single-scattering albedos, and asymmetry parameters for each layer.
CAM 3.0 includes a mechanism to scale the masses of each aerosol species by user-selectable factors at runtime. These factors are global, time-independent constants. This provides the flexibility to consider the climate effects of an arbitrary combination of the aerosol species in the climatology. It also facilitates simulation of climates different from present-day conditions for which the only information available is the ratio of globally averaged aerosol emissions or atmospheric loadings. A mechanism to scale the carbonaceous aerosols with a time-dependent unitless factor has been included to facilitate realistic simulations of the recent past.
CAM 3.0 also includes a run-time option for computing a diagnostic set of shortwave fluxes with an arbitrary combination of aerosols multiplied with a separate set of user-selectable scale factors. This option can be used to compute, for example, the aerosol radiative forcing relative to an atmosphere containing no aerosols.
The diagnostic fields produced the aerosol calculation include the
column-integrated optical depth and column-averaged single-scattering
albedo, asymmetry parameter, and forward scattering parameter (in the
-Eddington approximation) for each aerosol species and
spectral interval. These fields are only computed for illuminated grid
points, and for non-illuminated points the fields are set to zero.
The fraction of the time that a given grid point is illuminated is
also recorded. Time
averages of, for example, the optical depth can be obtained by
dividing the time-averaged optical depths in the history files by the
corresponding daylit fractions.
The option of introducing a globally uniform background sulfate aerosol is retained, although by default the optical depth of this aerosol is set to zero. Its optical properties are computed using the same sulfate optics as are used for the aerosol climatology. However, for consistency with the uniform aerosol in previous versions of CAM 3.0 and CCM3, the relative humidity used to compute hygroscopic growth is set to 80%.
An ice particle effective radius, , is also diagnosed by CAM 3.0.
Following Kristjánsson and Kristiansen [97], the effective radius for ice clouds
is now a function only of temperature, as shown in Figure 4.2.
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For cloud scattering and absorption, the radiative parameterization of
Slingo [160] for liquid water droplet clouds is employed. In this
parameterization, the optical properties of the cloud droplets are
represented in terms of the prognosed cloud water path (CWP, in units
of kg m) and effective radius
, where
is the cloud drop size distribution as a
function of radius
.
Cloud radiative properties explicitly account for the phase of
water. For shortwave radiation we use the following generalization of
the expression used by Slingo [160] for liquid water clouds. The
cloud liquid optical properties (extinction optical depth, single
scattering albedo, asymmetry parameter and forward scattering
parameter) for each spectral interval are defined as
The radiative properties of ice cloud are defined
by
The treatment of cloud vertical overlap follows Collins [38].
The overlap parameterization is designed to reproduce calculations
based upon the independent column approximation (ICA). The differences
between the results from the new parameterization and ICA are governed
by a set of parameters in the shortwave code
(Table 4.1 on page and
section 4.8.9). The differences can be made
arbitrarily small with appropriate settings of these parameters. The
current parameter settings represent a compromise between
computational cost and accuracy.
The new parameterizations can treat random, maximum, or an arbitrary combination of maximum and random overlap between clouds. The type of overlap is specified with the same two variables for the longwave and shortwave calculations. These variables are the number of random-overlap interfaces between adjacent groups of maximally-overlapped layers and a vector of the pressures at each of the interfaces. The specification of the overlap is completely separated from the radiative calculations, and if necessary the type of overlap can change at each grid cell or time step.
The algorithm for cloud overlap first converts the vertical profile of
partial cloudiness into an equivalent collection of binary cloud
configurations. Let
be the fractional amount of cloud in
layer
in a profile with
layers. The index
corresponds
to the top of the model atmosphere and
corresponds to the
layer adjacent to the surface. Let
be the number of
maximally-overlapped regions in the column separated by random-overlap
boundaries. If the entire column is maximally overlapped, then
, and if the entire column is randomly overlapped, then
.
Each region
includes all layers
between
and
.
Within each region, identify the
unique, non-zero cloud amounts
and sort them into a descending list
with
.
Note than in CAM 3.0, cloud amounts are not allowed to be identically
equal to 1. It is convenient to define
and
. By construction
for
.
The binary cloud configurations are defined in terms of the sorted
cloud amounts. The number of unique cloud binary configurations in
region is
. The
binary cloud
configuration
in region
is given by
The cloud overlap for radiative calculations in CAM 3.0 is
maximum-random (M/R). Clouds in adjacent layers are maximally
overlapped, and groups of clouds separated by one or more clear layers
are randomly overlapped. The two overlap parameters input to the
radiative calculations are the number of random-overlap interfaces,
which equals , and a vector of pressures
at each
random-overlap interface. These parameters are determined for each
grid cell at each radiation time step. Suppose there are
groups of vertically contiguous clouds in a given grid cell. The
first parameter
. Let
represent the pressure
at the bottom interface of each group of contiguous clouds, and let
denote the surface pressure. Both
and
increase from
the top of the model downward. Then
For diagnostic purposes, the CAM 3.0 calculates three levels of cloud
fraction assuming the same maximum-random overlap as in the radiative
calculations. These diagnostics, denoted as low, middle, and high
cloud, are bounded by the pressure levels to 700 mb, 700 mb to
400 mb, and 400 mb to the model top.
The solution for the shortwave fluxes is calculated by determining all
possible arrangements of binary clouds which are consistent with the
vertical profile of partial cloudiness, the overlap assumption, and
the parameters for accelerating the solution (Table 4.1
and section 4.8.9).
The shortwave radiation within each of these configurations is
calculated using the same -Eddington solver introduced in CCM3
[27]. The all-sky fluxes and heating rates for the
original profile of partial cloudiness are calculated as weighted sums
of the corresponding quantities from each configuration. The weights
are equal to the horizontal fractional area occupied by each
configuration. The number of configurations is given by
eqn. (4.200), and the area of each configuration is given
by eqn. (4.202). There are two steps in the calculations:
first, the calculation of the cloud-free and overcast radiative
properties for each layer, and second the combination of these
properties using the adding method to calculate fluxes. These two
processes are described below.
Details of the implementation are as follows. The CAM 3.0 model
atmosphere is divided into layers in the vertical; an extra top
layer (with index 0, above the
layers specified by CAM 3.0) is
added. This extra layer prevents excessive heating in the top layer
when the top pressure is not very low; also, as the model does not
specify absorber properties above its top layer, the optical
properties of the top layer must be used for the extra layer. In
CAM 3.0, clear-sky and all-sky solar fluxes are calculated and output
for the top of model (TOM) at layer 1 and the top of atmosphere (TOA)
corresponding to layer 0. The TOM fluxes are used to compute the
model energetic balance, and the TOA fluxes are output for diagnostic
comparison against satellite measurements. The provision of both sets
of fluxes is new in CAM 3.0. Layers are assumed to be horizontally and
vertically homogeneous for each model grid point and are bounded
vertically by layer interfaces. For each spectral band, upward and
downward fluxes are computed on the layer interfaces (which include
the surface and top interface). The spectral fluxes are summed and
differenced across layers to evaluate the solar heating rate. The
following discussion refers to each of the spectral intervals.
In general, several constituents absorb and/or scatter in each
homogeneous layer (e.g. cloud, aerosol, gases...). Every constituent
is defined in terms of a layer extinction optical depth , single
scattering albedo
, asymmetry parameter
, and the forward
scattering fraction
. To define bulk layer properties, the
combination formulas of Cess [30] are used:
The -Eddington solution for each layer requires scaled
properties for
,
,
, given by the expressions:
To combine layers, it is assumed that radiation, once scattered, is
diffuse and isotropic (including from the surface). For an arbitrary
layer 1 (or combination of layers with radiative properties
,
,
,
)
overlaying layer 2 (or combination of layers with radiative properties
,
, and
), the
combination formulas for direct and diffuse radiation incident from
above are:
Note that the transmissions for each layer (
)
and for the combined layers
are total transmissions,
containing both direct and diffuse transmission. Note also that the
two layers (or combination of layers), once combined, are no longer a
homogeneous system.
To combine the layers over the entire column, two passes are made through the layers, one starting from the top and proceeding downward, the other starting from the surface and proceeding upward. The result is that for every interface, the following combined reflectivities and transmissivities are available:
![]() |
direct beam transmission from top-of-atmosphere to the | |
interface (![]() |
||
to the interface), | ||
![]() |
reflectivity to direct solar radiation of entire atmosphere | |
below the interface, | ||
![]() |
total transmission to direct solar radiation incident from above | |
to entire atmosphere above the interface, | ||
![]() |
reflectivity of atmosphere below the interface to diffuse | |
radiation from above, | ||
![]() |
reflectivity of atmosphere above the interface to diffuse | |
radiation from below. |
With these quantities, the upward and downward fluxes at every
interface can be computed. For example, the upward flux would be the
directly transmitted flux (
) times the reflection
of the entire column below the interface to direct radiation
(
), plus the diffusely transmitted radiation from above
that reaches the interface (
)
times the reflectivity of the entire atmosphere below the interface to
diffuse radiation from above (
), all times a factor
that accounts for multiple reflections at the interface. A similar
derivation of the downward flux is straightforward. The resulting
expressions for the upward and downward flux are:
If two or more configurations of binary clouds are identical between
TOA and a particular interface, then
,
, and
are also identical at that interface. The adding
method is applied once and the three radiative quantities are copied
to all the identical configurations. This process is applied at each
interface by constructing a binary tree of identical cloud
configurations starting at TOA down to the surface. A similar method
is used for
and
, which are calculated using the adding
method starting the surface and continuing up to a particular
interface. The copying of identical radiative properties reduces the
number of calculations of
,
, and
by 62% and the
number of calculations of
and
by 21% in CAM 3.0 with M/R
overlap.
The computational cost of the shortwave code has two components: a
fixed cost for computing the radiative properties of each layer under
clear and overcast conditions, and a variable cost for applying the
adding method for each column configuration
. The
variable component can be reduced by omitting configurations which
contribute small terms in the shortwave fluxes. Several mechanisms
for selecting configurations for omission have been included in the
parameterization. The parameters that govern the selection process
are described in Table 4.1.
Any combination of the selection conditions may be imposed. If the
parameter
, cloud layers with
are
identified as cloud-free layers. The configurations including these
clouds are excluded from the flux calculations. If the parameter
, the cloud
amounts are discretized by