Lecture4.0_Intro_rad_trans

Introduction to radiative transfer : 

Introduction to radiative transfer Radiative transfer is the physical phenomenon of energy transfer in the form of electromagnetic radiation. The propagation of radiation through a medium is affected by absorption, emission and scattering processes. The equation of radiative transfer describes these interactions mathematically. Equations of radiative transfer have application in wide variety of subjects including optics, astrophysics, atmospheric science, and remote sensing. Analytic solutions to the radiative transfer equation (RTE) exist for simple cases, but for more realistic media with complex multiple scattering effects, numerical methods are required.

Electromagnetic spectrum : 

Electromagnetic spectrum

Planck’s spectral distribution law : 

Planck’s spectral distribution law Planck introduced in 1901 his hypothesis of quantized oscillators in a radiating body. He derived an expression for the hemispherical blackbody spectral radiative flux Where h is Planck’s constant, mr is the real index of refraction, kB is Boltzmann’s constant

Comparison of solar and Earth’s blackbody intensity : 

Comparison of solar and Earth’s blackbody intensity

UV-Visible Solar Spectrum : 

UV-Visible Solar Spectrum

IR flux from EarthSahara : 

IR flux from EarthSahara

Absorption in molecular lines and bands : 

Absorption in molecular lines and bands Molecules have three types of energy levels - electronic, vibrational, and rotational Transitions between electronic levels occur mainly in the ultraviolet Transitions between vibrational levels - visible/near IR Transitions between rotational levels - far IR/ mm wave region O2 and N2 have essentially no absorption in the IR 4 most important IR absorbers H2O, CO2, O3, CH4

Vibrational levels : 

Vibrational levels Consider a diatomic molecule. The two atoms are bound together by a force, and can oscillate along the axis of the molecule. The force between the two atoms is given by The solution of which is

Vibrational levels : 

Vibrational levels v0 is known as the vibrational frequency theoretically v0 can assume all values However in quantum mechanics these values must be discrete v is the vibrational quantum number

Vibrational levels : 

Vibrational levels In general k depends on the separation of the atoms and we have an ‘anharmonic oscillator’

Schematic of vibrational levels : 

Schematic of vibrational levels

Various forms of molecular vibration : 

Various forms of molecular vibration

Rotational levels : 

Rotational levels Consider a diatomic molecule with different atoms of mass m1 and m2, whose distance from the center of mass are r1 and r2 respectively The moment of inertia of the system about the center of mass is:

Rotational levels : 

Rotational levels The classical expression for energy of rotation is where J is the rotational quantum number

Vibrating Rotator : 

Vibrating Rotator If there were no interaction between the rotation and vibration, then the total energy of a quantum state would be the sum of the two energies. But there is, and we get The wavenumber of a spectral line is given by the difference of the term values of the two states

Energy levels of a vibrating rotator : 

Energy levels of a vibrating rotator

Fine structure in HCl : 

Fine structure in HCl

Intensity distribution in bands of HCl : 

Intensity distribution in bands of HCl

Line broadening : 

Line broadening Classical theory leads to the following equation for the shape of a line (transition). It is called the Lorentz profile Since the Lorentz profile is normalized we find by integrating over all frequencies

Line broadening : 

Line broadening The line width (full width at half maximum) of the Lorentz profile is the damping parameter, . For an isolated molecule the damping parameter can be interpreted as the inverse of the lifetime of the excited quantum state. This is consistent with the Heisenberg Uncertainty Principle If absorption line is dampened solely by the natural lifetime of the state, this is natural broadening

Pressure broadening : 

Pressure broadening For an isolated molecule the typical natural lifetime is about 10-8 s, 5x10-4 cm-1 line width Collisions between molecules can shorten this lifetime. These collisions can be viewed as ‘billiard ball’ reactions, or as the overlapping of the potential fields of the two molecules. The collision process leads to a Lorentz line shape.

Pressure broadening : 

Pressure broadening Clearly the line width will depend on the number of collisions per second, i.e., on the number density of the molecules (Pressure) and the relative speed of the molecules (the square root of the temperature)

Doppler broadening : 

Doppler broadening Second major source of line broadening Molecules are in motion when they absorb. This causes a change in the frequency of the incoming radiation as seen in the molecules frame of reference (Doppler effect) Let the velocity be v, and the incoming frequency be , then

Doppler broadening : 

Doppler broadening In the atmosphere the molecules are moving with velocities determined by the Maxwell Boltzmann distribution

Doppler broadening : 

Doppler broadening The cross section at a frequency is the sum of all line of sight components

Doppler broadening : 

Doppler broadening We now define the Doppler width as

Comparison of line shapes : 

Comparison of line shapes

The extinction law : 

The extinction law

Extinction Law : 

Extinction Law The extinction law can be written as The constant of proportionality is defined as the extinction coefficient. k can be defined by the length of the absorbing path with the gas at one atmosphere pressure

Optical depth : 

Optical depth Normally we are interested in the total extinction over a finite distance (path length) Where is the extinction optical depth The integrated form of the extinction equation becomes

Extinction = scattering + absorption : 

Extinction = scattering + absorption Extinction really consists of two distinct processes, scattering and absorption, hence where

Differential equation of radiative transfer : 

Differential equation of radiative transfer We must now add the process called emission. We introduce an emission coefficient, jν Combining the extinction law with the definition of the emission coefficient noting that

Differential equation of radiative transfer : 

Differential equation of radiative transfer The ratio jn/k(n) is known as the source function, This is the differential equation of radiative transfer

Scattering : 

Scattering Two types of scattering are considered – molecular scattering (Rayleigh) and scattering from aerosols (Mie) The equation for Rayleigh scattering can be written as where α is the polarizability

Rayleigh scattering : 

Rayleigh scattering Sky appears blue at noon, red at sunrise and sunset - why? Rayleigh scattering (named after the English physicist Lord Rayleigh) is the elastic scattering of light or other electromagnetic radiation by particles much smaller than the wavelength of the light, i.e., individual atoms or molecules. It can occur when light travels in transparent solids and liquids, but is most prominently seen in gases. Rayleigh scattering is a function of the electric polarizability of the particles, which describes how much the electrical charges on the molecule will move in an electric field.

Phase diagram for Rayleigh scattering : 

Phase diagram for Rayleigh scattering

Mie-Debye scattering : 

Mie-Debye scattering For particles which are not small compared with the wavelength one has to deal with multiple waves from different molecules/atoms within the particle Forward moving waves tend to be in phase and this gives a large resultant amplitude. Backward waves tend to be out of phase and this results in a small resultant amplitude Hence the scattering phase function for a particle has a much larger forward component (forward peak) than the backward component

Phase diagrams for aerosols : 

Phase diagrams for aerosols

Differential Equation of Radiative Transfer : 

Differential Equation of Radiative Transfer Introduce two additional parameters. B, the Planck function, and a , the single scattering albedo (the ratio of the scattering cross section to the extinction coefficient). The complete time-independent radiative transfer equation which includes both scattering and absorption is

Solution for Zero Scattering : 

Solution for Zero Scattering If there is no scattering, e.g. in the thermal infrared, then the equation becomes

Transmittance : 

Transmittance For monochromatic radiation the transmittance, T, is given simply by But now we must consider how to deal with radiation that is not monochromatic. In this case the integration must be made over all frequencies. Absorption cross section at high spectral resolution are available in tabular form – HITRAN. But usually an average value over a frequency interval is used.

Transmission in spectrally complex media : 

Transmission in spectrally complex media transmittance

Statistical Band Model (Goody) : 

Statistical Band Model (Goody) Goody studied the water-vapor bands and noted the apparent random line positions and band strengths. Let us assume that the interval Dn contains n lines of mean separation d, i.e. Dn=nd Let the probability that line i has a line strength Si be P(Si) where P is normally assumed to have a Poisson distribution

Statistical Band Model (Goody) : 

Statistical Band Model (Goody)

Statistical Band Model (Goody) : 

Statistical Band Model (Goody) We have reduced the parameters needed to calculate T to two These two parameters are either derived by fitting the values of T obtained from a line-by-line calculation, or from experimental data.

K distribution technique : 

K distribution technique

K distribution technique : 

K distribution technique

Two-stream Approximation- Isotropic Scattering : 

Two-stream Approximation- Isotropic Scattering Although anisotropic scattering is more realistic, let’s look at isotropic scattering i.e. p=1 The radiative transfer equations are

Two-stream Approximation- Isotropic Scattering : 

Two-stream Approximation- Isotropic Scattering In the two-stream approximation we replace the angular dependent quantities I by their averages over each hemisphere. This leads to the following pair of coupled differential equations

Two-stream Approximation- Isotropic Scattering : 

Two-stream Approximation- Isotropic Scattering If the medium is homogeneous then a is constant. One can now obtain analytic solutions to these equations. m in the above equations is the cosine of the average polar angle. It generally differs in the two hemispheres

Discrete Ordinate Method – Isotropic Scattering : 

Discrete Ordinate Method – Isotropic Scattering The solution of the isotropic scattering problem involves the following integral over angle In the two stream method we replaced the integration over m with the simple formula

Discrete Ordinate Method – Isotropic Scattering : 

Discrete Ordinate Method – Isotropic Scattering This is obviously a crude approximation. We can improve the accuracy by including more points in a numerical quadrature formula Where w’j is a quadrature weight, and uj is the discrete ordinate Most commonly used radiative transfer computer codes is DISORT – DIScreteOrdinateRadiativeTransfer