1 / 19

Lecture 5: Radiative transfer theory where light comes from and how it gets to where it’s going

Tuesday, 19 January 2010. Lecture 5: Radiative transfer theory where light comes from and how it gets to where it’s going. Reading. Ch 1.2 review, 1.3, 1.4 http://hyperphysics.phy-astr.gsu.edu/hbase/atmos/blusky.html (scattering)

alta
Télécharger la présentation

Lecture 5: Radiative transfer theory where light comes from and how it gets to where it’s going

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Tuesday, 19 January 2010 Lecture 5: Radiative transfer theory where light comes from and how it gets to where it’s going Reading Ch 1.2 review, 1.3, 1.4 http://hyperphysics.phy-astr.gsu.edu/hbase/atmos/blusky.html (scattering) http://id.mind.net/~zona/mstm/physics/light/rayOptics/refraction/refraction1.html (refraction) http://id.mind.net/~zona/mstm/physics/light/rayOptics/refraction/snellsLaw/snellsLaw1.html (Snell’s Law) Review On Solid Angles, (class website -- Ancillary folder: Steradian.ppt) Last lecture: color theory data spaces color mixtures absorption

  2. The Electromagnetic Spectrum (review) Units: Micrometer = 10-6 m Nanometer = 10-9 m Light emitted by the sun The Sun

  3. Light from Sun – Light Reflected and Emitted by Earth W m-2 μm -1 W m-2μm-1 sr-1 Wavelength, μm The sun is not an ideal blackbody – the 5800 K figure and graph are simplifications

  4. Atmospheric Constituents Constant Nitrogen (78.1%) Oxygen (21%) Argon (0.94%) Carbon Dioxide (0.033%) Neon Helium Krypton Xenon Hydrogen Methane Nitrous Oxide Variable Water Vapor (0 - 0.04%) Ozone (0 – 12x10-4%) Sulfur Dioxide Nitrogen Dioxide Ammonia Nitric Oxide All contribute to scattering For absorption, O2, O3, and N2 are important in the UV CO2 and H2O are important in the IR (NIR, MIR, TIR)

  5. Solar spectra before and after passage through the atmosphere

  6. Atmospheric transmission

  7. Modeling the atmosphere To calculate t we need to know how k in the Beer-Lambert-Bouguer Law (called b here) varies with altitude. Modtran models the atmosphere as thin homogeneous layers. Modtran calculates k or b for each layer using the vertical profile of temperature, pressure, and composition (like water vapor). This profile can be measured made using a balloon, or a standard atmosphere can be assumed. Fo is the incoming flux

  8. 20 15 10 5 0 20 15 10 5 0 Altitude (km) Altitude (km) 0 20 40 60 80 100 -80 -40 0 40 Relative Humidity (%) Temperature (oC) Radiosonde data Mt Everest Mt Rainier

  9. Radiant energy – Q (J) - electromagnetic energy Solar Irradiance – Itoa(W m-2) - Incoming radiation (quasi directional) from the sun at the top of the atmosphere. Irradiance – Ig (W m-2) - Incoming hemispheric radiation at ground. Comes from: 1) direct sunlight and 2) diffuse skylight (scattered by atmosphere). Downwelling sky irradiance – Is↓(W m-2) – hemispheric radiation at ground Path Radiance - Ls↑ (W m-2 sr-1 ) (Lpin text) - directionalradiation scattered into the camera from the atmosphere without touching the ground Transmissivity – t- the % of incident energy that passes through the atmosphere Radiance – L (W m-2 sr-1) – directional energy density from an object. Reflectance – r -The % of irradiance reflected by a body in all directions (hemispheric: r·I) or in a given direction (directional: r·I·p-1) Note: reflectance is sometimes considered to be the reflected radiance. In this class, its use is restricted to the % energy reflected. Terms and units used in radiative transfer calculations 0.5º Itoa L Ls↑ Is↓ Ig

  10. Radiative transfer equation Parameters that relate to instrument and atmospheric characteristics DN = a·Ig·r + b This is what we want Igis the irradiance on the ground r is the surface reflectance a & b are parameters that relate to instrument and atmospheric characteristics

  11. Radiative transfer equation DN = a·Ig·r + b DN = g·(te·r · ti·Itoa·cos(i)/p + te· r·Is↓/p + Ls↑) + o g amplifier gain t atmospheric transmissivity e emergent angle i incident angle r reflectance Itoa solar irradiance at top of atmosphere Ig solar irradiance at ground Is↓ down-welling sky irradiance Ls↑ up-welling sky (path) radiance o amplifier bias or offset

  12. Lambert The factor of p Consider a perfectly reflective (r=100%) diffuse “Lambertian” surface that reflects equally in all directions.

  13. The factor of p Consider a perfectly reflective (r=100%) diffuse “Lambertian” surface that reflects equally in all directions. If irradiance on the surface is Ig, then the irradiance from the surface is r·Ig = Ig W m-2. The radiance intercepted by a camera would be r·Ig/p W m-2 sr-1. The factor p is the ratio between the hemispheric radiance (irradiance) and the directional radiance. The area of the sky hemisphere is 2p sr (for a unit radius). So – why don’t we divide by 2p instead of p?

  14. p/2 p/2 2p 2p ∫ ∫ L sin  cos  d dw=pL ∫ ∫ sin  d dw=2p 0 0 0 0 • Incoming directional radiance L at elevation angle  is isotropic • Reflected directional radiance Lcos  is isotropic • Area of a unit hemisphere: The factor of p Consider a perfectly reflective (r=100%) diffuse “Lambertian” surface that reflects equally in all directions.

  15. Itoa Itoa cos(i) i Highlighted terms relate to the surface Ls↑ (Lp) ti te i e Ig=ti Itoa cos(i) r(ti Itoa cos(i)) /p reflected light r reflectance “Lambertian” surface

  16. Ls↑=r Is↓ /p Lambert Is↓ Measured Ltoa DN(Itoa) = a Itoa + b Itoa Ltoa=ter (ti Itoa cos(i))/p + te r Is↓ /p+ Ls↑ Itoa cos(i) i Highlighted terms relate to the surface Ls↑ (Lp) ti te i e Ig=ti Itoa cos(i) r(ti Itoa cos(i)) /p reflected light r reflectance “Lambertian” surface

  17. Next lecture: Atmospheric scattering and other effects Mauna Loa, Hawaii

More Related