Open access peer-reviewed chapter

Perturbation Method for Solar/Infrared Radiative Transfer in a Scattering Medium with Vertical Inhomogeneity in Internal Optical Properties

By Yi-Ning Shi, Feng Zhang, Jia-Ren Yan, Qiu-Run Yu and Jiangnan Li

Submitted: January 13th 2018Reviewed: April 10th 2018Published: November 5th 2018

DOI: 10.5772/intechopen.77147

Downloaded: 183

Abstract

A new scheme based on perturbation method is presented to solve the problem of solar/infrared radiative transfer (SRT/IRT) in a scattering medium, in which the inherent optical properties (IOPs) are vertically inhomogeneous. The Eddington approximation for SRT and the two-stream approximation for IRT are used as the zeroth-order solution, and multiple-scattering effect of inhomogeneous IOPs is included in the first-order solution. Observations show that the stratocumulus clouds are vertically inhomogeneous, and the accuracy of SRT/IRT for stratocumulus clouds by different solutions is evaluated. In the spectral band of 0.25–0.69 μm, the relative error in absorption with inhomogeneous SRT solution is 1.4% at most, but with the homogeneous SRT solution, it can be up to 7.4%. In the spectral band of 5–8 μm, the maximum relative error of downward emissivity can reach −11% for the homogeneous IRT solution but only −2% for the inhomogeneous IRT solution.

Keywords

  • perturbation method
  • radiative transfer
  • vertical inhomogeneity

1. Introduction

Solving the radiative transfer equation (RTE) is a key issue in radiation scheme for climate model and remote sensing. In most numerical radiative transfer algorithms, the atmosphere is divided into many homogeneous layers. The inherent optical properties (IOPs) are then fixed within each layer and the variations of IOPs inside each layer are ignored, effectively regarding each layer as internally homogeneous. The standard solar/infrared radiative transfer (SRT/IRT) solutions are based on this assumption of internal homogeneity [1, 2, 3, 4], which cannot resolve within-layer vertical inhomogeneity.

It has been well established by observation that cumulus and stratocumulus clouds (hereinafter, collectively referred to as cumulus clouds) are inhomogeneous, both horizontally and vertically [5, 6, 7, 8, 9]. Inside a cumulus cloud, the liquid water content (LWC) and the cloud droplet size distribution vary with height, and so the IOPs of cloud droplets depend on vertical height.

How to deal with vertical internal inhomogeneity in SRT/IRT models is an interesting topic for researchers. Li developed a Monte Carlo cloud model that can be used to investigate photon transport in inhomogeneous clouds by considering an internal variation of the optical properties [10]. Their model showed that when overcast clouds become broken clouds, the difference in reflectance at large solar zenith angles between vertically inhomogeneous clouds and their plane-parallel counterparts can be as much as 10%.

However, the Monte Carlo method is very expensive in computing and not applicable to climate models or remote sensing [11]. The albedo of inhomogeneous mixed-phase clouds at visible wavelengths could be obtained by using a Monte Carlo method to compare such clouds with plane-parallel homogeneous clouds [12].

In principle, the vertical inhomogeneity problem of the SRT/IRT process can be solved by increasing the number of layers of the climate model. However, it is time-consuming to increase the vertical resolution of a climate model. Typically, there are only 30–100 layers in a climate model [13], which is not high enough to resolve the cloud vertical inhomogeneity. To completely address the problem of vertical inhomogeneity by using a limited number of layers in a climate model, the standard SRT method must be extended to deal with the vertical inhomogeneity inside each model layer. The primary purpose of this study is to introduce a new inhomogeneous SRT/IRT solution presented by Zhang and Shi. This solution follows a perturbation method: the zeroth-order solution is the standard Eddington approximation for SRT and two-stream approximation for IRT, with a first-order perturbation to account for the inhomogeneity effect. In Section 2, the basic theory of SRT/IRT is introduced, and the new inhomogeneous SRT/IRT solution is presented. In Section 3, the inhomogeneous SRT/IRT solution is applied to cloud as realistic examples to demonstrate the practicality of this new method. A summary is given in Section 4.

2. SRT/IRT solution for an inhomogeneous layer

2.1. SRT solution

The azimuthally averaged solar radiative transfer equation [1, 2, 3, 4, 10, 11, 12] is

μdISτμ=ISτμωτ211ISτμPτμμdμωτ4πF0Pτμμ0eτμ0E1

where μ is the cosine of the zenith angle (μ > 0 and μ < 0 refer to upward and downward radiation, respectively), Pτμμis the scattering phase function, τis the optical depth (τ=0and τ=τ0refer to the top and bottom of the medium, respectively), ωτis the single-scattering albedo, and F0is the incoming solar flux. For the Eddington approximation, Pτμμ=1+3gτμμ(−1 < μ <1) and gτare the asymmetry factors. For the scattering atmosphere, the irradiance fluxes in the upward and downward directions can be written as

FS±τ=2π0±1ISτμμdμE2

To simulate a realistic medium such as cloud or snow, we consider ωτand gτto vary with τ, and we use exponential expressions here to simplify the process. The single-scattering albedo and asymmetry factor are written as

ωτ=ω̂+εωea1τea1τ0/2E3a
gτ=ĝ+εgea2τea2τ0/2E3b

where τ0is the optical depth of the layer, ω̂is the single-scattering albedo at τ0/2, and ĝis the asymmetry factor at the same place. Both εgand εωare small parameters that are far less than ĝand ω̂, respectively, in a realistic medium.

According to the Eddington approximation, the radiative intensity ISτμcan be written as

ISτμ=IS0τ+IS1τμE4

Using Eqs. (1), (2), and (4), we obtain

dFS+τ=γ1τFS+τγ2τFSτγ3τωτF0eτμ0E5a
dFSτ=γ2τFS+τγ1τFSτ+1γ3τωτF0eτμ0E5b
FS0=0,FS+τ0=RdifFSτ0+Rdirμ0F0eτ0μ0E5c

where γ1τ=1474+3gτωτ, γ2τ=14143gτωτ, and γ3τ=1423gτμ0; τ0is the optical depth of the single layer; and Rdif(Rdir) is the diffuse (resp., direct) reflection from the layer below or the diffuse (direct) surface albedo. Substituting γ1τ, γ2τ, and γ3τinto Eq. (3) and ignoring the small second-order parameters εω2, εg2, and εωεg, we get

γ1τ=γ10+γ11εωea1τea1τ0/2+γ12εgea2τea2τ0/2E6a
γ2τ=γ20+γ21εωea1τea1τ0/2+γ22εgea2τea2τ0/2E6b
γ3τ=γ30+γ32εgea2τea2τ0/2E6c

where γ10=1474+3ĝω̂, γ20=14143ĝω̂, γ30=1423ĝμ0, γ11=144+3ĝ, γ12=34ω̂, γ21=1443ĝ, γ22=34ω̂, and γ32=34μ0.

By perturbation theory [14], the corresponding flux can also be expanded by using the perturbation coefficients εωand εg:

FS+=FS0++εωFS1++εgFS2+E7a
FS=FS0+εωFS1+εgFS2E7b

Substituting Eqs. (6) and (7) into Eq. (5) yields

dFS+=γ10+γ11εωea1τea1τ0/2+γ12εgea2τea2τ0/2FS0++εωFS1++εgFS2+γ20+γ21εωea1τea1τ0/2+γ22εgea2τea2τ0/2FS0+εωFS1+εgFS2ω̂γ30+γ30εωea1τea1τ0/2+ω̂γ32εgea2τea2τ0/2F0eτμ0E8a
dFS=γ20+γ21εωea1τea1τ0/2+γ22εgea2τea2τ0/2FS0++εωFS1++εgFS2+γ10+γ11εωea1τea1τ0/2+γ12εgea2τea2τ0/2FS0+εωFS1+εgFS2+ω̂γ40+γ40εωea1τea1τ0/2ω̂γ32εgea2τea2τ0/2F0eτμ0E8b

where γ40=1γ30. And, Eq. (8) can be rewritten as separate equations for FS0±, FS1±, and FS2±. We obtain the following equations for the scattered flux FS0±:

dFS0+=γ10FS0+γ20FS0γ30ω̂F0eτμ0E9a
dFS0=γ20FS0+γ10FS0+γ40ω̂F0eτμ0E9b
FS00=0,FS0+τ0=RdifFS0τ0+Rdirμ0F0eτ0μ0E9c

Eq. (9) is the standard SRT equation for a homogeneous layer [15] and has the following solution:

FS0+=K1e+ΓK2e+G1eτμ0E10a
FS0=ΓK1e+K2e+G2eτμ0E10b

where K1=ΓRdifΓG2ekτ0G1RdirG2Rdirμ0F0eτ0μ01RdifΓekτ0ΓRdifΓekτ0, K2=ΓK1G2, G1=γ301μ0γ10γ20γ40μ02ω̂F01μ02k2, G2=γ401μ0+γ10+γ20γ30μ02ω̂F01μ02k2, Γ=12kγ10+γ20+k, and k2=γ10+γ20γ10γ20. And, the equations for the perturbation terms FSi±(i = 1, 2) are

dFSi+=γ10FSi+γ20FSi+eaiτeaiτ0/2γ1iFS0+γ2iFS0γ3i1F0eaiτeaiτ0/2eτμ0E11a
dFSi=γ20FSi+γ10FSi+eaiτeaiτ0/2γ2iFS0+γ1iFS0γ4i1F0eaiτeaiτ0/2eτμ0E11b
FSi0=0,FSi+τ0=RdifFSiτ0E11c

where γ31=γ41=ω̂γ32. Letting Mi=FSi++FSiand Ni=FSi+FSi, Eq. (11a) and (11b) yields

dMi=γ10+γ20Ni+ψi++ψiek+aiτ+ζi++ζiekaiτ+χi++χieai+1μ0τeaiτ0/2ψi++ψie+ζi++ζie+χi++χieτμ0E12a
dNi=γ10γ20Mi+ψi+ψiek+aiτ+ζi+ζiekaiτ+χi+χieai+1μ0τeaiτ0/2ψi+ψie+ζi+ζie+χi+χieτμ0E12b

where Ψi+=K2γ1iΓγ2i, Ψi=K2γ2iΓγ1i, ζi+=K1γ1iγ2iΓ, ζi=K1γ2iγ1iΓ, χi+=γ1iG1γ2iG2γ3i1F0, and χi=γ2iG1γ1iG2+γ4i1F0.

From Eq. (12), we obtain

d2Midτ2=k2Mi+η1i+ek+aiτ+η2i+ekaiτ+η3i+eai+1μ0τ+η4i+e+η5i+e+η6i+eτμ0E13a
d2Nidτ2=k2Ni+η1iek+aiτ+η2iekaiτ+η3ieai+1μ0τ+η4ie+η5ie+η6ieτμ0E13b

where η1i±=γ10±γ20ψi+ψik+aiψi+±ψi, η2i±=kaiζi+±ζi+γ10±γ20ζi+ζi, η3i±=χi+χiγ10±γ20ai+1μ0χi+χi, η4i±=eaiτ0/2γ10±γ20ψi+ψikψi+±ψi, η5i±=eaiτ0/2kζi+±ζi+γ10±γ20ζi+ζi, and η6i±=eaiτ0/2χi+χiγ10±γ201μ0χi+χi.

The solutions of Eq. (13) are

Mi=Ai+e+Bi+e+Pi+ek+aiτ+Qi+ekaiτ+Ri+eai+1μ0τη4i+2ke+η5i+2ke+η6i+μ021μ02k2eτμ0E14a
Ni=Aie+Bie+Piek+aiτ+Qiekaiτ+Rieai+1μ0τη4i2ke+η5i2ke+η6iμ021μ02k2eτμ0E14b

where Pi±=η1i±k+ai2k2, Qi±=η2i±kai2k2, and Ri±=η3i±ai+1μ02k2eτμ0. Finally, we can obtain FSiand FSi+as

FSi+=D1i+e+D2i+e+φ1i+ek+aiτ+φ2i+ekaiτ+φ3i+eai+1μ0τ+φ4i+τek1τ+φ5i+τe+φ6i+eτμ0E15a
FSi=D1ie+D2ie+φ1iek+aiτ+φ2iekaiτ+φ3ieai+1μ0τ+φ4iτek1τ+φ5iτe+φ6ieτμ0E15b

where D1i±=Ai+α±Xi, D2i±=Bi+α±±Y, α±=121±kγ10+γ20, Xi=eaiτ0/2ψi++ψi2γ10+γ20η4i+4kγ10+γ20,

Yi=eaiτ0/2ζi++ζi2γ10+γ20+η5i+4kγ10+γ20, ϕ1i±=12Pi+±Pi, ϕ2i±=12Qi+±Qi, ϕ3i±=12Ri+±Ri, ϕ4i±=η4i+±η4i4k, ϕ5i±=η5i+±η5i4k, and ϕ6i±=η6i+±η6iμ021μ02k2. Biand Aiare determined by the boundary conditions as

Bi+=ϕ1i+ϕ2i+ϕ3i+ϕ6i)αRdifα+ekτ0+α+ϕ1i+Rdifϕ1iek+aiτ0+ϕ2i+Rdifϕ2iekaiτ0ααRdifα+ekτ0α+α+Rdifαekτ0+α+ϕ3i+Rdifϕ3ieai+1μ0τ0+ϕ4i+Rdifϕ4i)τ0ekτ0+ϕ5i+Rdifϕ5iτ0ekτ0+ϕ6i+Rdifϕ6ieτ0μ0]ααRdifα+ekτ0α+α+Rdifαekτ0+Xi+YiαRdifα+ekτ0+Xi+RdifXiα+ekτ0+Yi+RdifYiα+ekτ0ααRdifα+ekτ0α+α+Rdifαekτ0E16a
Ai+=1α+Xi+YiBiαϕ1iϕ2iϕ3iϕ6iE16b

All detailed calculation about solar radiation can be found at [16].

2.2. IRT solution

The azimuthally averaged infrared radiative transfer equation for intensity IIτμis [1, 2, 3, 4, 10, 11, 12]

μdIIτμ=IIτμωτ211IIτμPτμμ'dμ'1ωτBTE17

where μ, τ, Pτμμ', and ωτare same as in Eq. (1). BTis the Planck function at temperature T, which represents the internal infrared emission of the medium.

The Planck function is approximated lineally as a function of optical depth [2] as

BTτ=B0+βτE18

where β=B1B0/τ0and τ0are the total optical depth of the medium. The Planck functions B0and B1are evaluated by using the temperature of the top (τ=0) and the bottom (τ=τ0) of the medium.

According to the two-stream approximation, the intensities can be written as IIτμ1=II+τand IIτμ1=IIτ, respectively, where μ1=μ1=1/1.66is a diffuse factor that converts radiative intensity to flux [17]. 11IIτμPτμμdμcan be written as

11IIτμPτμμdμ=1+3gτμμ1II+τ+1+3gτμμ1IIτE19

where gτis the asymmetry factor.

Using Eqs. (17) and (19), we can obtain

dII+τ=γ1τII+τγ2τIIτγ3τBτE20a
dII+τ=γ2τII+τγ1τIIτ+γ3τBτE20b

where γ1τ=1ωτ1+gτ/2μ1, γ2τ=ωτ1gτ2μ1, and γ3τ=1ωτμ1.

For IRT, we also use Eq. (3) to represent an inhomogeneous medium such as cloud or snow, in which ωτand gτvary with τ. By substituting Eq. (3) into γ1τ, γ2τ, and γ3τand by ignoring the second order of the small parameters of εω2, εg2, and εωεg, we can obtain

γ1τ=γ10+γ11εωea1τea1τ0/2+γ12εgea2τea2τ0/2E21a
γ2τ=γ20+γ21εωea1τea1τ0/2+γ22εgea2τea2τ0/2E21b
γ3τ=γ30+γ31εωea1τea1τ0/2E21c

In the above formula, γi0, γi1, and γi2(i = 1, 2, 3) are the known factors of ω̂and ĝ. These known factors are introduced for simplifying original expressions, in which γ10=1ω̂1+ĝ/2μ1, γ20=ω̂1ĝ2μ1, γ30=1ω̂μ1, γ11=1+ĝ2μ1, γ21=1ĝ2μ1, γ31=1μ1, γ12=γ22=ω̂2μ1, and γ32=0.

Same as in Eq. (7), the upward and downward intensity can be written as

II+=II0++εωII1++εgII1+E22a
II=II0+εωII1+εgII1E22b

By substituting Eqs. (21)(22) into Eq. (20), we obtain

dII+=γ10+γ11εωea1τea1τ0/2+γ12εgea2τea2τ0/2II0++εωII1++εgII2+γ20+γ21εωea1τea1τ0/2+γ22εgea2τea2τ0/2II0+εωII1+εgII2γ30+γ31εωea1τea1τ0/2BτE23a
dIIdτ=γ20+γ21εωea1τea1τ0/2+γ22εgea2τea2τ0/2II0++εωII1++εgII2+γ10+γ11εωea1τea1τ0/2+γ12εgea2τea2τ0/2II0+εωII1+εgII2+γ30+γ31εωea1τea1τ0/2BτE23b

By removing the second-order and higher-order perturbation terms, we can also separate Eq. (23) into three equations of IIi±(i = 0, 1, 2). The equations of II0±can be written as

dII0+=γ10dII0+γ20dII0γ30BτE24a
dII0=γ20II0+γ10II0+γ30BτE24b
II00=0,II0+τ0=1εsII0τ0+εsBTsE24c

where Tsand εsare surface temperature and surface emissivity, respectively. Eq. (24) is the standard homogeneous two-stream infrared radiative transfer equation [3, 15] with solutions

II0+=α+K0ekτ0τ+αH0e+G1τ+G2+E25a
II0=αK0ekτ0τ+α+H0e+G1τ+G2E25b

where k2=γ10+γ20γ10γ20, α±=121±kγ10+γ20, G1=γ30γ10γ20β, G2±=γ30γ10γ20B0±βγ30k2, H0=αekτ0G2+RG2+1RG1τ01RBTsα+RαG2α+α+RαααRdifα+e2kτ0, K0=α+H0+G2αekτ0, and R=1εs.

The equations for IIi±(i = 1, 2) are

dIIi+=γ10IIi+γ20IIi+eaiτeaiτ0/2γ1iII0+γ2iII0γ3iBτE26a
dIIi=γ20IIi+γ10IIi+eaiτeaiτ0/2γ2iII0+γ1iII0+γ3iBτE26b
IIi0=0,IIi+τ0=1εsIIiτ0E26c

Let Mi=IIi++IIiand Ni=IIi+IIi. Eq. (26a) and (26b) yields

dMi=γ10+γ20Ni+χ1i+ekτ0+kaiτ+χ2i+ek+aiτ+χ3i+ekτ0τ+χ4i+e+χ5i++χ6i+eaiτE27a
dNi=γ10γ20Mi+χ1iekτ0+kaiτ+χ2iek+aiτ+χ3iekτ0τ+χ4ie+χ5i+χ6ieaiτ+χ7iτ+χ8iτeaiτE27b

where χ1i±=K0α+αγ1i±γ2i, χ2i±=H0α+αγ1i±γ2i, χ3i±=K0α+αγ1i±γ2ieaiτ0/2, χ4i±=±H0α+αγ1i±γ2ieaiτ0/2, χ5i+=G2+G2γ1i+γ2ieaiτ0/2, χ5i=G2++G2γ1iγ2ieaiτ0/2+2B0γ3ieaiτ0/2, χ6i+=G2+G2γ1i+γ2i, χ6i=G2++G2γ1iγ2i2B0γ3i, χ7i=2G1γ1iγ2i+2βγ3ieaiτ0/2, and χ8i=2G1γ1iγ2i2βγ3i.

From Eq. (27), we can obtain

d2Midτ2=k2Mi+ϕ1i+ekτ0+kaiτ+ϕ2i+ek+aiτ+ϕ3i+ekτ0τ+ϕ4i+e+ϕ5i++ϕ6i+eaiτ+ϕ7i+τ+ϕ8i+τeaiτE28a
d2Nidτ2=k2Ni+ϕ1iekτ0+kaiτ+ϕ2iek+aiτ+ϕ3iekτ0τ+ϕ4ie+ϕ5i+ϕ6ieaiτ+ϕ8iτeaiτE28b

where ϕ1i±=γ10±γ20χ1i+kaiχ1i±, ϕ2i±=γ10±γ20χ2ik+aiχ2i±, ϕ3i±=γ10±γ20χ3i+kχ3i±, ϕ4i±=γ10±γ20χ4ikχ4i±, ϕ5i+=γ10+γ20χ5i, ϕ5i=γ10γ20χ5i++χ7i, ϕ6i+=γ10+γ20χ6iaiχ6i+, ϕ6i=γ10γ20χ6i+aiχ6i+χ8i, ϕ7i+=γ10+γ20χ7i, ϕ8i+=γ10+γ20χ8i, and ϕ8i=aiχ8i. Thus, the solutions are

Mi=K1iekτ0τ+H1ie+P1i+ekτ0+kaiτ+P2i+ek+aiτ+P3i+τekτ0τ+P4i+τe+P5i++P6i+eaiτ+P7i+τ+P8i+τeaiτE29a
Ni=K2iekτ0τ+H2ie+P1iekτ0+kaiτ+P2iek+aiτ+P3iτekτ0τ+P4iτe+P5i+P6ieaiτ+P8iτeaiτE29b

where P1i±=ϕ1i±kai2k2, P2i±=ϕ2i±k+ai2k2, P3i±=ϕ3i±2k, P4i±=ϕ4i±2k, P5i±=ϕ5i±k2, P6i±=ϕ6i±ai2k2+2aiϕ8i±ai2k22, P7i+=ϕ7i+k2, and P8i+=ϕ8i+ai2k2.

The expressions of IIi±are

IIi+=D1i+ekτ0τ+D2i+e+σ1i+ekτ0+kaiτ+σ2i+ek+aiτ+σ3i+τekτ0τ+σ4i+τe+σ5i++σ6i+eaiτ+σ7iτ+σ8i+τeaiτE30a
IIi=D1iekτ0τ+D2ie+σ1iekτ0+kaiτ+σ2iek+aiτ+σ3iτekτ0τ+σ4iτe+σ5i+σ6ieaiτ+σ7iτ+σ8iτeaiτE30b

where D1i±=K1iα±±Xi, D2i±=H1iα±Yi, Xi=P3i+χ3i+2γ10+γ20, Yi=P4i+χ4i+2γ10+γ20, σji±=12Pji+±Pji. (j = 1, 2, 3, 4, 5, 6, 8), σ7i=12P7i+, and K1iand H1iare determined by boundary conditions. By substituting Eq. (30) into the boundary conditions of Eq. (26c), we can obtain

H1i=α+RαXiekτ0+Yiσ1iekτ0σ2iσ5iσ6i+αekτ0R+1Xi+R+1Yiekτ0α+α+RdifαααRdifαe2kτ0αekτ0Rσ1iσ1i+eaiτ0+Rσ2iσ2i+ek+aiτ0+Rσ3iσ3i+τ0+Rσ4iσ4i+τ0ekτ0α+α+RdifαααRdifαe2kτ0αekτ0Rσ5iσ5i++Rσ6iσ6i+eaiτ0+R1σ7iτ0+Rσ8iσ8i+τ0eaiτ0α+α+RdifαααRdifαe2kτ0E31a
K1i=1αekτ0Xiekτ0+Yiα+H1iσ1iekτ0σ2iσ5iσ6iE31b

Finally, the upward and downward fluxes are obtained by

FI+0=πII+0E32a
FIτ0=πIIτ0E32b

All detailed calculation about solar radiation can be found at [18].

3. Results and discussion

We apply the two schemes to idealized medium to investigate its accuracy, and the result has been shown on [16] and [18].

For true cloud medium, because ice clouds' optical properties strongly depend on the complex particle habits [19, 20, 21]. Therefore, we limit our discussion here to water cloud only. According to the observation, the internal LWC (g m−3) and droplet radius of the cloud tend to increase with height [22]. To take this feature into account, LWC and droplet cross-sectional area (DCA; cm−2, m−3) should increase linearly from the cloud base to the position near the top of the cloud:

LWC=0.22+0.00008zE33a
DCA=100+zE33b

where 0 < z < z0. The terms z and z0 denote the height from the cloud base and the height of the cloud top, respectively. From Eq. (33a) to (33b), the cloud effective radius (re; μm) and liquid water path (LWP; g m−2) can be obtained:

rez=34ρLWCDCA1010E34a
LWP=0z0LWCdzE34b

where ρ (g m−3) is the liquid water density. In this case, LWC varies from 0.22 to 0.30 g m−3, and revaries from 2.06 to 16.50 μm, in which both ranges are consistent with observation [23]. According to [24], we choose LWP = 260 (g m−2) to represent low cloud. In the benchmark calculations, z0 is divided into 100 internal homogeneous sub-layers, although other numbers can be chosen (e.g., 200). In principle, more internal sub-layers should result in more accurate results. We use 100 internal sub-layers throughout this study because having any more makes little difference to the calculated results. Using 100 sub-layers are sufficiently accurate to resolve the vertical internal inhomogeneity of the medium. We use the optical properties of a water cloud in the solar spectral band of 0.25–0.69 μm and at 0.94 μm and in the infrared spectral band of 5–8 μm and 11 μm.

In Figure 1a and b, the benchmark values of the inhomogeneous IOPs and the parameterized results for the spectral band of 0.25–0.69 μm are shown. The parameterized inhomogeneous IOPs are

1ωτ=3.979×1071.897×106e0.1539τe0.1539τ0/2E35a
gτ=0.8359+0.0289e0.1539τe0.1539τ0/2E35b

where τ0=110.84. The corresponding results for reflection and absorption are shown in Figure 1cf. For reflection, the relative error with the homogeneous solution increases from 0.25 to 0.71% as μ0 increases from 0.01 to 1, whereas the relative error with the inhomogeneous solution increases from 0.05 to 0.14%. For absorption, the relative error is not sensitive to μ0; it is around 7.4% with the homogeneous solution but around only 1.4% with the inhomogeneous solution.

Figure 1.

For the band of 0.25–0.69 μm, (a-b) show cloud asymmetry factor/single-scattering albedo versus cloud optical depth (a for asymmetry factor; b for single-scattering albedo), (c-d) show the reflectance/absorptance versus solar zenith angle (c for reflectance; d for absorptance) and (e-f) show the relative errors of the homogeneous and inhomogeneous solutions (e for reflectance error, f for absorptance error).

In Figure 2a and b, the benchmark values of the inhomogeneous IOPs and the parameterized results for the wavelength 0.94 μm are shown. The parameterized inhomogeneous IOPs are

1ωτ=1.936×1045.263×104e0.0357τe0.0357τ0/2E36a
gτ=0.83210.0403e0.0218τe0.0218τ0/2E36b

where τ0=54.46. Figure 2cf shows the corresponding results for reflection and absorption. For reflection, the relative error with the homogeneous solution increases from 1.1 to 3.0% as μ0 increases from 0.01 to 1, whereas the relative error with the inhomogeneous solution increases from 0.7 to 2.0%. For absorption, the relative error is not sensitive to μ0; it is around 10% with the homogeneous solution but around only 5.7% with the inhomogeneous solution.

Figure 2.

Same as Figure 1 but for the wavelength 0.94 μm.

The benchmark values of IOPs and parameterized results for the band of 5–8 μm are shown in Figure 3a and b. Here, we assume

ωτ=0.67570.3697e0.0142τe0.0142τ0/2E37a
gτ=0.8644+0.1023e0.0155τe0.0155τ0/2E37b

where τ0=55.85. For upward emissivity (Figure 3c and d), the relative errors of both solutions are not sensitive to FI+τ0; the errors are around −3% for homogeneous solution and around 1% for inhomogeneous solution. For downward emissivity (Figure 3e and f), the relative error of homogeneous solution is 4% when FI+τ0=0, while the error of inhomogeneous solution is only 1%. With FI+τ0increasing from 0 to 5πBT, the error of homogeneous solution decreases to 0 firstly but then negatively increases to around −10%. The error of inhomogeneous solution shows a similar decreasing-increasing pattern, but the negative increase only reaches about −2%.

Figure 3.

For the band of 5-8 μm, (a-b) show the cloud single-scattering albedo and asymmetry factor versus cloud optical depth, black dots represent the exact values and the blue lines is the fitting results (a for single-scattering albedo; b for asymmetry factor); (c-d) show the upward/downward emissivity versus the ratio of the radiation incident from the bottom to the internal infrared emission of the medium (c for upward emissivity; d for downward emissivity) and (e-f) show the relative errors of the homogeneous and inhomogeneous solutions (e for upward emissivity; f for downward emissivity).

The benchmark values of IOPs and parameterized results for the band of 11 μm are shown in Figure 4a and b. In this case, we assume

ωτ=0.46230.2155e0.1018τe0.1018τ0/2E38a
gτ=0.91180.0083e0.1087τe0.1087τ0/2E38b

where τ0=28.23. For upward emissivity (Figure 4c and d), the relative error of homogeneous solution is −1.2%, while the error of inhomogeneous solution is less than 0.5%. For downward emissivity (Figure 4e and f), with FI+τ0increasing from 0 to 5πBT, the error of homogeneous (inhomogeneous) solution varies from 3 to −11% (from 0 to −1%).

Figure 4.

Same as Figure 3 but for the wavelength of 11 μm.

4. Summary and conclusions

In the above, we have considered the vertically inhomogeneous structures of only cloud and snow, whereas all physical quantities in the atmosphere are vertically inhomogeneous (e.g., the concentrations of all types of gases and aerosols). In current climate models, the vertical layer resolution is far from that required to resolve such vertical inhomogeneity. In this study, we have proposed a new inhomogeneous SRT/IRT solution to address the vertical inhomogeneity by introducing an internal variation of IOPs inside each model layer. This scheme is based on standard perturbation theory and allows us to use the standard solar Eddington solution and standard infrared two-stream solution for homogeneous layers to identify a zeroth-order equation and a first-order equation that includes the inhomogeneous effect. The new SRT/IRT solution can accurately express the inhomogeneous effect in each model layer, and it reduces to the standard solution when the medium is homogeneous.

The new inhomogeneous SRT/IRT solution is a good way to resolve cloud vertical inhomogeneity. In the spectral band of 0.25–0.69 μm, the relative error in the inhomogeneous SRT solution is no more than 1.4%, whereas the error with the homogeneous SRT solution can be up to 7.4%. At the specific wavelength of 0.94 μm, the relative error with the inhomogeneous solution is not more than 5.7% but can be up to 10% with the homogeneous SRT solution. In the band of 5–8 μm, the homogeneous IRT solution is not sensitive to FI+τ0, and its relative error may reach −3.2% for upward emissivity, whereas the error of inhomogeneous IRT solution is only 1%. With FI+τ0increasing from 0 to 5πBT, the error of downward emissivity for homogeneous solution varies from 4 to −10%, while the error ranges from 1 to −2% for inhomogeneous IRT solution. In the band of 11 μm, the relative error of homogeneous IRT solution is around −1.2% for upward emissivity, and the error of inhomogeneous IRT solution is only less than 0.5%. For downward emissivity, the maximum error of homogeneous IRT solution can be up to −11%, and the maximum error of inhomogeneous IRT solution is only around −1% when FI+τ0=5πBT.

In specific spectral bands or at particular wavelengths, the vertical variations in IOPs can typically be fitted easily into Eq. (3) to obtain the required parameters. A simple fitting program can be easily incorporated into a climate model to produce the inhomogeneous IOPs of stratocumulus clouds. If no such cloud inhomogeneity information is available in the current climate models, the vertical variation rates of cloud LWC and DCA can be derived empirically from observations, which show that the vertical variation rates of LWC and DCA in stratocumulus clouds are not very different [5, 7, 8].

In this study, we presented only a single-layer inhomogeneous SRT/IRT solution. To implement the new solution in a climate model, the adding process for layer-to-layer connections has to be solved. Under the homogeneous condition, the single-layer result in reflection and transmission is the same for an upward path and a downward path, but this is not true for an inhomogeneous layer. Therefore, the adding process has to be modified. We will present an algorithm for this multilayer adding process in our next study, in which the climatic impact of inhomogeneous clouds and inhomogeneous snows will be explored. The code base for the inhomogeneous SRT/IRT solution is available from the authors upon request.

Acknowledgments

The work is supported by National Natural Science Foundation of China (41675003) and the Priority Academic Program Development of Jiangsu Higher Education Institutions (PAPD).

© 2018 The Author(s). Licensee IntechOpen. This chapter is distributed under the terms of the Creative Commons Attribution 3.0 License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

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Yi-Ning Shi, Feng Zhang, Jia-Ren Yan, Qiu-Run Yu and Jiangnan Li (November 5th 2018). Perturbation Method for Solar/Infrared Radiative Transfer in a Scattering Medium with Vertical Inhomogeneity in Internal Optical Properties, Perturbation Methods with Applications in Science and Engineering, İlkay Bakırtaş, IntechOpen, DOI: 10.5772/intechopen.77147. Available from:

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