Remote Sensing in Geology, Siegal & Gillespie (class website) Wednesday, 26 January 2010 Lecture 7: Lambert’s law & reflection Interaction of light and surfaces Reading 2.4.3 – 2.6.4 spectra & energy interactions (p. 13-20) in: Remote Sensing in Geology, Siegal & Gillespie (class website) Previous lecture: atmospheric effects, scattering

What was covered in the previous lecture Friday’s lecture: Atmospheric scattering and other effects - where light comes from and how it gets there - we will trace radiation from its source to camera - the atmosphere and its effect on light - the basic radiative transfer equation: DN = a·Ig·r + b LECTURES Jan 05 1. Intro Jan 07 2. Images Jan 12 3. Photointerpretation Jan 14 4. Color theory Jan 19 5. Radiative transfer Jan 21 6. Atmospheric scattering previous Jan 26 7. Lambert’s Law today Jan 28 8. Volume interactions Feb 02 9. Spectroscopy Feb 04 10. Satellites & Review Feb 09 11. Midterm Feb 11 12. Image processing Feb 16 13. Spectral mixture analysis Feb 18 14. Classification Feb 23 15. Radar & Lidar Feb 25 16. Thermal infrared Mar 02 17. Mars spectroscopy (Matt Smith) Mar 04 18. Forest remote sensing (Van Kane) Mar 09 19. Thermal modeling (Iryna Danilina) Mar 11 20. Review Mar 16 21. Final Exam Today 1) reflection/refraction of light from surfaces (surface interactions) 2) volume interactions - resonance - electronic interactions - vibrational interactions 3) spectroscopy - continuum vs. resonance bands - spectral “mining” - continuum analysis 4) spectra of common Earth-surface materials Specifically: Reflection/refraction of light from surfaces (surface interactions) the RAT law Beer’s Law, Fresnel’s Law, Snell’s Law, Lambert’s Law Refraction, refractive index Reflection Types of surfaces, including Lambertian Scattering and scattering envelopes Topographic effects and shade Particle size effects 2

Light is reflected, absorbed , or transmitted (RAT Law) The amount of specular (mirror) reflection is given by Fresnel’s Law Fresnel’s law rs (n-1) 2 + K2 (n+1) 2 + K2 rs = n = refractive index K = extinction coefficient for the solid rs = fraction of light reflected from the 1st surface Mineral grain Absorption occurs here Transmitted component Beer’s law: (L = Lo e-kz) Snell’s law: n1·sin1 =n2·sin2 z = thickness of absorbing material k = absorption coefficient for the solid Lo = incoming directional radiance L = outgoing radiance Light passing from one medium to another is refracted according to Snell’s Law n = c/v

Refraction through a prism: absorptivity k is a function of l

Everyone discovered Snell’s Law (1621) Ibn Sahl (Baghdad, 984) On Burning Mirrors and Lenses Ptolemy (90-168 AD) Thomas Harriot, 1602 Willebrod Snel van Royen (Snell), 1621 Renée Descartes, 1637 Christian Huygens, 1678

Fresnel’s Law describes the reflection rs of light from a surface Augustin Fresnel Fresnel lens Fresnel’s Law describes the reflection rs of light from a surface rs = ---------------- (n -1)2 +K 2 n is the refractive index K is the extinction coefficient (n+1)2 +K 2 This is the specular ray K is not exactly the same as k, the absorption coefficient in Beer’s law (I = Io e-kz) (Beer – Lambert – Bouguer Law) K and k are related but not identical: k = --------- 4pK K is the imaginary part of the complex index of refraction: m=n-jK l

Fresnel’s Law… is more complicated than shown. The full formulation accounts for variation in angles i and e

Complex refractive index n* = n + i K Consider an electrical wave propagating in the x direction: Ex=E0,x·exp[i·(kx·x·-ωt)] kx = component of the wave vector in the x direction = 2p/l w = circular frequency =2pn; v=c/n* = n·λ v = speed in light in medium c = speed of light in vacuum k=2p/l=w·n*/c Substituting, Ex = E0,x·exp[i·(w·(n+i·K)/c·x·-ω·t)] Ex = E0,x·exp[(i·w·n·x/c-w· K·x/c-i·ω·t)] Ex = E0,x·exp[-w· K·x/c]·exp[(i·(kx·x·-ω·t))] If we use a complex index of refraction, the propagation of electromagnetic waves in a material is whatever it would be for a simple real index of refraction times a damping factor (first term) that decreases the amplitude exponentially as a function of x. Notice the resemblance of the damping factor to the Beer-Lambert-Bouguer absorption law. The imaginary part K of the complex index of refraction thus describes the attenuation of electromagnetic waves in the material considered.

- diffuse or Lambertian Surfaces may be - specular - back-reflecting - forward-reflecting - diffuse or Lambertian Smooth surfaces (rms<<l) generally are specular or forward-reflecting examples: water, ice Rough surfaces (rms>>l) generally are diffuse example: sand Complex surfaces with smooth facets at a variety of orientations are forward- or back-reflecting example: leaves Reflection envelopes

These styles of reflection from a surface con-trast with scattering within the atmosphere diffuse reflection forward scattering Types of scattering envelopes Uniform scattering Forward scattering Back scattering

Forward scattering/reflection in snow When light encounters a grain of snow it may scatter from sharp corners, reflect from the grain surface, or be transmitted through the grain. The effect is that light penetrates into a snow field and appears to be reflected diffusely from the surface. , but the actual mechanisms involve mainly transmission and refraction . The signature of this process is the observation that the “reflected” light may be colored by the bottoms of objects on the snow – example, skis. snow Light escapes from snow because the absorption coefficient k in e-kz is small This helps increase the “reflectivity” of snow Snow grain ski You can easily test this: observe the apparent color of the snow next to a ski or snowboard with a brightly colored base: What do you see?

How does viewing and illumination geometry affect radiance from Lambertian surfaces? The total irradiance intercepted by an extended surface is the same, but flux density is reduced by 1/cos i --- the total flux per unit area of surface is smaller by cos i Unit area Illumination I i I cos i i is the incident angle ; I is irradiance in W m-2

How does viewing and illumination geometry affect radiance from Lambertian surfaces? Unresolved surface element exactly fills the IFOV at nadir, but doesn’t off nadir – part of the pixel “sees” the background instead Viewer at zenith Viewer at viewing angle e angular IFOV Same IFOV For a viewer off zenith, the same pixel is not filled by the 1 m2 surface element and the measured radiance is L = r p-1 I cos i cos e therefore, point sources look darker as e increases 1 m2 Viewer at zenith sees r p-1 I cos i W sr-1 per pixel

How does viewing and illumination geometry affect radiance from Lambertian surfaces? Resolved surface element - pixels are filled regardless of e. Viewer at zenith Viewer at viewing angle e angular IFOV Same IFOV For a viewer off zenith, the same pixel now sees a foreshortened surface element with an area of 1/cos e m2 so that the measured radiance is L = r p-1 I cos i therefore, point sources do not change lightness as e increases 1 m2 Viewer at zenith still sees r p-1 I cos i W sr-1 per pixel

How does viewing and illumination geometry affect radiance from Lambertian surfaces? Reflection I i r p R= I cos i e I cos i i is the incident angle ; I is irradiance in W m-2 e is the emergent angle; R is the radiance in W m -2 sr-1

Lambertian Surfaces Specular ray I i i r p L= I cos i e I cos i i is the incidence angle; I is irradiance in W m-2 e is the emergence angle; L is the radiance in W m -2 sr-1 Specular ray would be at e=i if surface were smooth like glass

Rough at the wavelength of light Plowed fields Lambertian Surfaces Rough at the wavelength of light Plowed fields L= I cos i r p Lambertian surface - L is independent of e The total light (hemispherical radiance) reflected from a surface is L = r I cos i W m -2

the brightness of a snow field doesn’t depend on e, the exit angle DN=231 239 231 231 239 231 222

Reprise: reflection/refraction of light from surfaces (surface interactions) e i i Specular ray Incident ray Reflected light ° amount of reflected light = r I cos i ° amount is independent of view angle e ° color of specularly reflected light is essentially unchanged ° color of the refracted ray is subject to selective absorption ° volume scattering permits some of the refracted ray to reach the camera Refracted ray

{ Effect of topography is to change incidence angle i’ r L= I cos i’ p For topography elements >> l and >> IFOV i’ r p L= I cos i’ i { This is how shaded relief maps are calculated (“hillshade”) Shadow

Effect of topography is to change incidence angle For topography elements >> l and >> IFOV i’ r p L= I cos i’ i Image intensity Shadow For a nadir view

“Shadow,” “Shade” & “Shading” Shadow – blocking of direct illumination from the sun Shading - darkening of a surface due to illumination geometry. Does not include shadow. Shade – darkening of a surface due to shading & shadow combined i Variable shaded surfaces Shadowed Surface i’ 29

Confusion of topographic shading and unresolved shadows 33

- particle size effects - interaction mechanisms Next we’ll consider spectroscopy fundamentals - what happens to light as it is refracted into the surface and absorbed - particle size effects - interaction mechanisms Light enters a translucent solid - uniform refractive index Light enters a particulate layer - contrast in refractive index

Surface/volume ratio = lower Light from coarsely particulate surfaces will have a smaller fraction of specularly reflected light than light from finely particulate surfaces Surface/volume ratio = higher

Obsidian Spectra Finest Coarsest (Rock) Reflectance Wavelength (nm) mesh Rock 16-32 32-42 42-60 60-100 100-150 150-200

Next lecture: 1) reflection/refraction of light from surfaces (surface interactions) 2) volume interactions - resonance - electronic interactions - vibrational interactions 3) spectroscopy - continuum vs. resonance bands - spectral “mining” - continuum analysis 4) spectra of common Earth-surface materials