solar radiation and environmental biophysicslees.geo.msu.edu/courses/geo827/lecture_6b.pdfgeo 827...
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Solar Radiation and Environmental BiophysicsGeo 827, MSU
Jiquan ChenOct. 6, 2015
1) Solar radiation basics
2) Energy balance
3) Other relevant biophysics
4) A few selected applications of RS in ecosystem studies
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1) Fundamental solar radiation
Dr. Brian C. Ancell
Assistant Professor
Atmospheric Science Group
Department of Geosciences
Texas Tech University
On Oct. 5, Slides 2-x were
downloaded from
http://www.atmo.ttu.edu/bancell/
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• Energy is defined as
the ability to do work
1) Fundamental solar radiation
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Energy
• Energy is defined as
the ability to do work
• Kinetic energy – the
energy of motion
• Potential energy –
energy that can be
used
• Energy is conserved! (1st law of thermodynamics)
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Energy Transfer
• Although energy is conserved, it can
move through the following mechanisms:
1) Conduction – heat transfer by physical
contact, from higher to lower temperature
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Conduction in the Atmosphere
• Occurs at the atmosphere/surface
interface
• Partly responsible for daytime heating/nighttime
cooling! (The diurnal cycle)
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Energy Transfer
• Although energy is conserved, it can
move through the following mechanisms:
2) Convection – heat transfer by movement
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Convection in the Atmosphere
• Vertical transport of heat
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Convection in the Atmosphere
• Vertical transport of heat
• Horizontal transport of heat = advection
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Convection in the Atmosphere
Courtesy maltaweather.info
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Energy Transfer
• Although energy is conserved, it can
move through the following mechanisms:
3) Radiation - transfer of
energy by electromagnetic
radiation (no medium
required!)
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Radiation
Characteristics of radiation1) Wavelength – the distance between wave crests
2) Amplitude – the height of the wave
3) Wave speed – constant! (speed of light - 186,000
miles/second)
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Radiation
• The wavelength of radiation determines its type
• The amplitude determines the intensity
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Radiation
• What emits radiation? EVERYTHING!!
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Radiation
• The types (wavelengths) and intensity
(amplitudes) of radiation depend on temperature
Sun is HOT (~10,000oF) Earth is NOT (~59oF)
Shortwave radiation Longwave radiation
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Radiation
• Blackbody – an object that absorbs all radiation and
emits the maximum amount of radiation at every
wavelength (not realistic)
• Graybody – an object that emits a fraction (emissivity)
of blackbody radiation (more realistic)
• Total radiation emitted is equal to the sum over all
wavelengths above
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Radiation Laws
• Stefan-Boltzmann Law – the total amount of
blackbody radiation emitted (I) is related to
temperature:
I = σT4
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Radiation Laws
• Stefan-Boltzmann Law – the total amount of
blackbody radiation emitted (I) is related to
temperature:
I = σT4
• For a graybody, this becomes:
I = εσT4
where ε is the emissivity
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Radiation Laws
• Wien’s Law – the wavelength of maximum
blackbody emission is related to temperature:
ʎmax = 2900/T
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Radiation Laws
• Wien’s Law – the wavelength of maximum
blackbody emission is related to temperature:
ʎmax = 2900/T
Sun is HOT (~6000K) Earth is NOT (~290 K)
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GEO 827 – Digital Image Processing and Analysis
21
Typical atmospheric transmittance in VIS-SWIR
From Schowengerdt bookFall 2015
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Absorption Spectra of Atmospheric Gases
Anthes, p. 55
CH4
CO2
N2O
H2O
O2 & O3
atmosphere
WAVELENGTH (micrometers)
Infrared
Visible
UV
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Practical use of Radiation
Properties
• Visible satellite imagery doesn’t work in the dark
• Infrared (longwave) radiation occurs always –
use infrared satellite imagery!
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Solar Radiation and the Earth
• The solar constant – the amount of solar
radiation hitting the earth
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Solar Radiation and the Earth
Earth – 1367 W/m2
Mars – 445 W/m2
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Solar Radiation and the Earth
• Earth’s tilt is the true cause of the seasons!• Earth’s axis is tilted 23.5o
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Solar Radiation and the Earth
• 3 factors contribute to
the amount of incoming
solar radiation
(insolation):
1) Period of daylight
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Period of Daylight
Vernal and autumnal equinox
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Period of Daylight
Summer solstice
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Period of Daylight
Winter solstice
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Solar Radiation and the Earth
• 3 factors contribute to
the amount of incoming
solar radiation
(insolation):
2) Solar angle
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Solar Angle
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Solar Radiation and the Earth
• 3 factors contribute to
the amount of incoming
solar radiation
(insolation):
3) Beam depletion
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Beam Depletion
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Planetary Albedo
• A fraction of the incoming solar radiation (S) is reflected back into space, the rest is absorbed by the planet. Each planet has a different reflectivity, or albedo (α):
– Earth α = 0.31 (31% reflected, 69% absorbed)
– Mars α = 0.15
– Venus α = 0.59
– Mercury α = 0.1
• Net incoming solar radiation = S(1 - α)
• One possible way of changing Earth’s climate is by changing its albedo.
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Land has
higher
albedo than
ocean
Clouds have
high albedo
Ice and snow
have high
albedo
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Principles of Terrestrial
Ecosystem Ecology
Chapin, Matson and Vitousek
2nd edition, 2011
Chapter 4
Water and Energy Balance
2) Energy balance
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Chapin et al., 2011 Fig. 4.28/30/11
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Energy balance equation
39
0/ tQAGLEHLK w
where:
K net shortwave radiation
L net longwave radiation
LE latent heat transfer
H sensible heat transfer
G soil flux
Aw advective energy
ΔQ/Δt change in stored energy
Units: [EL-2T-1]
Bowen ratio = H/LE replace H = B∙LE
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2) Other relevant biophysicsReflection of land surface
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Seeing (infra)Red
Chlorophyll strongly absorbs radiation in the red and blue wavelengths
but reflects green wavelengths. (This is why healthy vegetation appears
green.)
The internal structure of healthy leaves act as excellent diffuse reflectors
of near-infrared wavelengths.
Measuring and monitoring the near-IR reflectance is one way that
scientists can determine how healthy (or unhealthy) vegetation may be.
Anita Davis & Jeannie Allen
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Spectral information:
vegetation
Wavelength, nm
400 600 800 1000 1200
refle
cta
nce
(%)
0.0
0.1
0.2
0.3
0.4
0.5
very high leaf area
very low leaf area
sunlit soil
NIR, high
reflectance
Visible red, low
reflectance
Visible green,
higher than red
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Vegetation characteristics
• high reflectivity in
NIR
• - distinguish
between vegetation
types on basis of
spectral reflection
curves
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Spectral signatureExplain why water looks darkish blue; Explain why vegetation looks
greenish; Explain why sand looks reddish yellow
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Atmospheric temperaturehttp://lightning.sbs.ohio-state.edu/geog1900/ch4_pressure_wind1.ppt(4 slides)
2) Other relevant biophysics
Vertical temperature
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Temperature Basics
• Temperature – measure of average kinetic energy
(motion) of individual molecules in matter
• Three temperature scales (units): Kelvin (K), Celsius (C), Fahrenheit (F)
– All scales are relative
– degrees F = 9⁄5 degrees C + 32
– degrees K = degrees C + 273.15
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Temperature Layers
Due to surface heating (Longwave, Latent heat, Sensible heat)
Due to ozone absorption of sunlight
Due to Solar winds, Cosmic rays
Decreasing rate w/ height (Lapse rate):6.5 oC/km
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An artist’s view
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49
• Pressure-temperature relation (Ideal gas law)
• Adiabatic lapse rate (dry & wet)
• Vapour – Vapour pressure, ea
– Sat. vapour pressure, ea*
– Absolute humidity, ρv
– Specific humidity, q = ρa/ρv
– Relative humidity, Wa = ea/ea*
– Dew point temperature, Td
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50
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies
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4) A few selected applications of RS in ecosystem studies