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ElectroMagnetic Radiation (EMR) Lecture 3  August 9, 2006
Ways of Energy Transfer Energy  is the ability to do work. In the process of doing work, energy is often transferred from one body to another or from one place to another. The three basic ways in which energy can be transferred include  conduction ,  convection , and  radiation . •  Most people are familiar with  conduction  which occurs when one body (molecule or atom) transfers its kinetic energy to another by colliding with it ( physical contact ). This is how a pan gets heated on a stove.  •  In  convection , the kinetic energy of bodies is transferred from one place to another by  physically moving the bodies . A good example is the convectional heating of air in the atmosphere in the early afternoon (less dense air rises).  •  The transfer of energy by  electromagnetic radiation   is of primary interest to remote sensing because it is the only form of energy transfer that can take place  in a vacuum  such as the region between the Sun and the Earth. Jensen, 2000
Remote sensing and EMR ,[object Object]
Source: Stan Aronoff, 2005 MGS TES 6 – 50  µm
1. Describe the EMR ,[object Object],[object Object]
1A. Wave model ,[object Object],Jensen, 2000
Three characteristics of electromagnetic wave  ,[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],The  amplitude  of an electromagnetic wave is the  height of the wave crest above the undisturbed position Travel time from the Sun to Earth is 8 minutes
EMR details ,[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],Bees and some other insects can see near UV. The Sun is the source of UV, but only > 0.3   m  (near UV) can reach the Earth .
EMR details (2)
1B. Particle model ,[object Object],[object Object],[object Object],[object Object],[object Object],Newton’s experiment in 1966
Energy of quanta (photons) Jensen, 2000
2. Source of EMR ,[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],Jensen, 2000
Jensen, 2000
3.Paths and Interactions ,[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],Jensen, 2000 60 miles
3A. Energy-Matter interactions in the atmosphere ,[object Object]
Atmospheric refraction (transmission) ,[object Object],Jensen, 2000 n i  = c/c i n i  index of refraction c speed of light in a vacuum c i  speed of light in a substance
Atmospheric scattering ,[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object]
Absorption ,[object Object],[object Object],[object Object],[object Object],[object Object]
Absorptions by atmospheric gasses The absorption of the Sun's incident electromagnetic energy in the region from 0.1 to 30   m by various atmospheric gasses. The first four graphs depict the absorption characteristics of N 2 0, 0 2  and 0 3 , CO 2 , and H 2 O. The final graphic depicts the cumulative result of having all these constituents in the atmosphere at one time. The atmosphere essentially closes down in certain portions of the spectrum while there exist “atmospheric windows” in other regions that transmit incident energy effectively to the ground. It is within these windows that remote sensing systems function, including 0.3-2.4, 3-5, 8-14   m, and > 0.6 cm. Most of these windows become less transparent when air is moist; clouds absorb most of longer wave emitted from the Earth, that is why cloudy nights tend to be warmer than clear nights. Only >0.9 cm can penetrating clouds close down Atmospheric window
Energy reaches the Earth after absorptions or blockage Source: Stan Aronoff, 2005
 
Reflectance ,[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object]
Specular versus diffuse reflectance
[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],3B. Energy-Matter interactions with the terrain
Selected reflectance curves Jensen, 2000
Some Results Source: X. Zhou et al. 1 2 3  4  5  7
[object Object],[object Object],[object Object],Wavenumber ( ν )  = 1/ λ ,  λ  is wavelength ( µ m).  traditionally,  ν  is expressed in inverse cm, so  ν  = 10 4 / λ   (cm -1 )
Solid angle ,[object Object],[object Object],[object Object],Ω  = A / r 2
Concept of radiance sr: steradian θ   is the zenith angle
[object Object],3C. Energy-Matter interactions in the atmosphere once again
[object Object],[object Object],[object Object],3D. Energy-Matter interactions in the sensor system
Jensen, 2000 ,[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object],[object Object]

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L3 emr

  • 1. ElectroMagnetic Radiation (EMR) Lecture 3 August 9, 2006
  • 2. Ways of Energy Transfer Energy is the ability to do work. In the process of doing work, energy is often transferred from one body to another or from one place to another. The three basic ways in which energy can be transferred include conduction , convection , and radiation . • Most people are familiar with conduction which occurs when one body (molecule or atom) transfers its kinetic energy to another by colliding with it ( physical contact ). This is how a pan gets heated on a stove. • In convection , the kinetic energy of bodies is transferred from one place to another by physically moving the bodies . A good example is the convectional heating of air in the atmosphere in the early afternoon (less dense air rises). • The transfer of energy by electromagnetic radiation is of primary interest to remote sensing because it is the only form of energy transfer that can take place in a vacuum such as the region between the Sun and the Earth. Jensen, 2000
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  • 4. Source: Stan Aronoff, 2005 MGS TES 6 – 50 µm
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  • 11. Energy of quanta (photons) Jensen, 2000
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  • 19. Absorptions by atmospheric gasses The absorption of the Sun's incident electromagnetic energy in the region from 0.1 to 30  m by various atmospheric gasses. The first four graphs depict the absorption characteristics of N 2 0, 0 2 and 0 3 , CO 2 , and H 2 O. The final graphic depicts the cumulative result of having all these constituents in the atmosphere at one time. The atmosphere essentially closes down in certain portions of the spectrum while there exist “atmospheric windows” in other regions that transmit incident energy effectively to the ground. It is within these windows that remote sensing systems function, including 0.3-2.4, 3-5, 8-14  m, and > 0.6 cm. Most of these windows become less transparent when air is moist; clouds absorb most of longer wave emitted from the Earth, that is why cloudy nights tend to be warmer than clear nights. Only >0.9 cm can penetrating clouds close down Atmospheric window
  • 20. Energy reaches the Earth after absorptions or blockage Source: Stan Aronoff, 2005
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  • 23. Specular versus diffuse reflectance
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  • 26. Some Results Source: X. Zhou et al. 1 2 3 4 5 7
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  • 29. Concept of radiance sr: steradian θ is the zenith angle
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Editor's Notes

  1. The amplitude of an electromagnetic wave is the height of the wave crest above the undisturbed position
  2. -273 c or 0 K
  3. shrub keep more energy