1. Week Four Principles of EMR and how EMR is used to perform RS
Energy transfer processes: conduction, convection, radiation
Fundamental EMR interactions
EMR properties: wavelength (λ), frequency (ν), amplitude (A)
Major divisions of the electromagnetic spectrum
EMR models
Wave: c = λν, Stefan-Boltzmann law, Wien's displacement law
Particle: quanta / quantum leap / photon
Energy / matter interactions in the atmosphere
Refraction
Scattering
Absorption
Reflectance
Energy / matter interactions with the terrain
Radiation budget equation: radiant flux (Φ) incoming (incident) to terrain must be accounted for
Ratios of radiant flux (Φ) for reflectance, absorptance, and transmittance
Radiant flux (Φ) density exitance
Radiance (L): projected radiant flux density leaving at a specific direction and specific solid angle
Energy / matter interactions in the atmosphere - again
Energy / matter interactions at the sensor

2. Gamma rays <0.03 nm X-rays 0.03 – 300 nm
UV radiation – 0.38 μm
Visible light – 0.72 μm
Infrared
Near-infrared – 1.30 μm
Mid-infrared – 3.00 μm
Far-infrared – 1,000 μm (1 mm)
Microwave 1 mm – 30 cm
Radio ≥ 30 cm
Image from: John R. Jensen  Introduction to Remote Sensing, 2nd Edition. NJ: Pearson Prentice Hall.

3. From temp., determine dominant wavelength (λ) using Wien’s displacement law: λmax = k / T
From temp., determine total emitted radiation (M) using Stephan-Boltzmann law: Mλ = σ T4
Image from: James B. Campbell  Introduction to Remote Sensing, 4th Edition. NY: Guilford Publications.

4. Image from: James B. Campbell. 2007
Image from: James B. Campbell  Introduction to Remote Sensing, 4th Edition. NY: Guilford Publications.

5. Image from: John R. Jensen. 2007
Image from: John R. Jensen  Introduction to Remote Sensing, 2nd Edition. NJ: Pearson Prentice Hall.