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EE 543 Theory and Principles of Remote Sensing

O. Kilic EE 543. 2. Outline. IntroductionRadiometric QuantitiesBrightnessPower, power densitySpectral BrightnessSpectral PowerSpectral Flux DensitySummary of Radiometric DefinitionsThermal RadiationPower-Temperature CorrespondenceNon-Blackbody RadiationAntenna Efficiency Considerations

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EE 543 Theory and Principles of Remote Sensing

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    1. 1 EE 543 Theory and Principles of Remote Sensing Introduction to Radiometry

    2. O. Kilic EE 543 2 Outline Introduction Radiometric Quantities Brightness Power, power density Spectral Brightness Spectral Power Spectral Flux Density Summary of Radiometric Definitions Thermal Radiation Power-Temperature Correspondence Non-Blackbody Radiation Antenna Efficiency Considerations

    3. O. Kilic EE 543 3 Summary So far we have discussed how waves interact with their surroundings: Wave equation Lossy medium Plane waves, propagation Reflection and transmission We have also discussed how waves are generated and received by antennas, studied the fundamental principles of antenna theory. Now we will build on our understanding of antennas and em radiation to investigate principles of radiometry.

    4. O. Kilic EE 543 4 What is Radiometry? Radiometry is the field of science related to the measurement of electromagnetic radiation. It is concerned with the measurement of incoherent radiation. Passive form of remote sensing; i.e. a natural source, such as Sun, provides the available radiation.

    5. O. Kilic EE 543 5 Introduction All matter radiate (=emit) electromagnetic energy. The bulk of energy received by earth is in the form of solar electromagnetic radiation. Part of the incident solar energy is scattered and absorbed by the atmosphere; the remainder is transmitted to the earth’s surface.

    6. Characteristics of Solar Radiation The surface temperature of Sun is 5,750-6,000 K and radiates energy across a range of wavelengths. Its distance to earth is about 150 million km (vacuum), only 5x109 % reaches earth. It then travels 100 km long atmosphere to reach the surface. 99% of the solar energy is within 0.28-4.96 mm waveband, most of it in infrared. O. Kilic EE 543 6

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