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Transcript of Photochemistry of Atmospheric Species Photolysis Reactions Molecular Spectra and Quantum Yields...
![Page 1: Photochemistry of Atmospheric Species Photolysis Reactions Molecular Spectra and Quantum Yields Solar Radiation Fundamentals of Radiative Transfer Aerosols.](https://reader035.fdocuments.in/reader035/viewer/2022070413/5697bfd31a28abf838cac5a8/html5/thumbnails/1.jpg)
Photochemistry of Atmospheric Species
Photolysis ReactionsMolecular Spectra and Quantum YieldsSolar Radiation
Fundamentals of Radiative TransferAerosolsClouds
Radiative Forcing of ClimateBiological Effects of UV Radiation
Sasha MadronichNational Center for Atmospheric ResearchBoulder Colorado [email protected], 8 February 2011
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Energetics of Oxygen in the Atmosphere
DHf (298K) kcal mol-1
Excited atoms O*(1D) 104.9
Ground state atoms O (3P) 59.6
Ozone O3 34.1
Normal molecules O2 0
2
Increasingstability
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Atmospheric OxygenThermodynamic vs. Actual
1E-110
1E-100
1E-90
1E-80
1E-70
1E-60
1E-50
1E-40
1E-30
1E-20
1E-10
1
200 220 240 260 280 300
Temperature, K
Co
nc
en
tra
tio
n, a
tm. O2 (=0.21)
thermodyn. O3
thermodyn. O
thermodyn. O*
observed O3
inferred O
inferred O*
3
O3
O
O*
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Photochemistry
Thermodynamics alone cannot explain atmospheric amounts of O3, O, O*
Need – energy input, e.g.
O2 + hn O + O (l < 240 nm)
– chemical reactions, e.g. O + O2 (+ M) O3 (+ M)
= Photochemistry
4
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Some Important Photolysis Reactions
O2 + hn (l < 240 nm) O + O source of O3 in stratosphere
O3 + hn (l < 340 nm) O2 + O(1D) source of OH in troposphere
NO2 + hn (l < 420 nm) NO + O(3P) source of O3 in troposphere
CH2O + hn (l < 330 nm) H + HCO source of HOx, everywhere
H2O2 + hn (l < 360 nm) OH + OH source of OH in remote atm.
HONO + hn (l < 400 nm) OH + NO source of radicals in urban atm.
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Quantifying Photolysis Processes
6
Photolysis reaction: AB + hn A + B
Photolysis frequency (s-1) J = l F(l) ( ) ( )s l f l dl
(other names: photo-dissociation rate coefficient, J-value)
Photolysis rates:
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CALCULATION OF PHOTOLYSIS COEFFICIENTS
J (s-1) = l F(l) ( ) ( )s l f l dl
F(l) = spectral actinic flux, quanta cm-2 s-1 nm-1
probability of photon near molecule.
( ) = s l absorption cross section, cm2 molec-1
probability that photon is absorbed.
( ) = f l photodissociation quantum yield, molec quanta-1
probability that absorbed photon causes dissociation.
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Measurement of Absorption Cross Section s(l)
8
Pressuregage
Pump forclean out
Gas in
Gas supply
Transmittance = I / Io = exp(-s n L)
s = -1/(nL) ln( I/Io )
Easy: measure pressure (n = P/RT), and relative change in light: I/Io
Light detector
Lamp
Prism
L
Absorption cell
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O2 Absorption Cross Section
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O3 Absorption Cross Section
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H2O2 Absorption Cross Section
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NO2 Absorption Cross Section
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CH2O Absorption Cross Section
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Measurement of Quantum Yields f(l)
14
L
Pressuregage
Pump forclean out
Gas in
Gas supply
Light detector
Transmittance = I / Io = exp(-s n L)
Quantum Yield = number of breaks per photon absorbedf = Dn / DI
Difficult: must measure absolute change in n (products) and I (photons absorbed)
Lamp
Prism
Absorption cell
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Measured Quantum Yields
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Compilations of Cross Sections & Quantum Yields
16
http://www.atmosphere.mpg.de/enid/2295
http://jpldataeval.jpl.nasa.gov/
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Spectral Range ForTropospheric Photochemistry
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
280 300 320 340 360 380 400 420
Wavelength, nm
dJ
/dl
(re
l)
O3->O2+O1D
NO2->NO+O
H2O2->2OH
HONO->HO+NO
CH2O->H+HCO
surface, overhead sun
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Solar Spectrum
UNEP, 2002
O2 and O3 absorball UV-C (l<280 nm)before it reaches the troposphere
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Typical Vertical Optical Depths, t
0.01
0.1
1
10
100
280 300 320 340 360 380 400 420
Wavelength, nm
Op
tic
al d
ep
th O3 (300 DU)
Rayleigh
Aerosol (25 km)
Cloud (32)
Direct transmission = exp(-t)Diffuse transmission can be much larger
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DIFFUSE LIGHT - CLEAN SKIES, SEA LEVEL
0.0
0.2
0.4
0.6
0.8
1.0
0 20 40 60 80 100
Solar zenith angle, deg.
Diff
use
frac
tion 320 nm
550 nm
Irradiance Actinic flux
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RADIATIVE TRANSFER CONCEPTS
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RADIATIVE TRANSFER THEORY…is hard
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Spectral Radiance, I
I( , ,l q f) = N(hc/l) / (dt dA dw dl) units: J s-1 m-2 sr-1 nm-1
(old name = spectral Intensity)
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INTEGRALS OVER ANGULAR INCIDENCE
24
2
0
2
0
ddsincos),(IE
0
2
0
ddsin),(IF
Watts m-2 Watts m-2 or quanta s-1 cm-2
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Absorption and Scattering
• Absorption – inelastic, loss of radiant energy:
• Scattering – elastic, radiant energy is conserved, direction changes:
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Beer-Lambert Law
Volume of box = V = Area x Thickness = A dz
Molecules (or particles):each has cross sectional area stotal number = N = n Vtotal area of molecules = s N = s n A dz
Fraction of light lost = fraction of area shaded by molecules = s n A dz / A = s n dz
Fraction of light surviving box:I(z+dz)/I(z) = 1 - s n dz
or [I(z+dz) - I(z)] / dz = - s n I(z)
or (lim dz 0)(differential form) dI/dz = - s n I(integral form) I(z2) = I(z1) exp [- s n (z2-z1)]
z z+dz
I(z) I(z+dz)
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Definition of Optical Depth
Beer-Lambert Law: I(z2) = I(z1) exp [- s n (z2-z1)]
Optical depth: t = s n (z2-z1)
If s and/or n depend on z, then
2
1
d)()(z
z
zznz
In monochromatic radiative transfer, t is often used as the spatial coordinate (instead of z)
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SCATTERING PHASE FUNCTIONS
P( , q f; q’, f’)
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The Radiative Transfer Equation
cos dI (, , )
d I ( , , )
o
4 F e
/ cos o P( , ;o,
o)
o
4I( , ' , ' )P (, ; ' , ' )1
10
2 d cos ' d '
Propagation derivative Beer-Lambert attenuation
Scattering fromdirect solar beam
Scattering from diffuse light(multiple scattering)
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NUMERICAL SOLUTIONS TO RADIATIVE TRANSFER EQUATION
• Discrete ordinates n-streams (n = even), angular distribution exact as n but speed 1/n2
• Two-stream family delta-Eddington, many others very fast but not exact
• Monte Carlo slow, but ideal for 3D problems
• Others matrix operator, Feautrier, adding-doubling,
successive orders, etc.
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Multiple Atmospheric LayersEach Assumed to be Homogeneous
Optical depth, DtSingle scattering albedo, wo = scatt./(scatt.+abs.)Asymmetry factor, g: forward fraction, f ~ (1+g)/2
Must specify three optical properties:
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For each layer, must specify Dt, wo, g:
1. Vertical optical depth, Dt(l, z) = s(l, z) n(z) Dz
for molecules: Dt(l, z) ~ 0 - 30Rayleigh scatt. ~ 0.1 - 1.0 ~ l-4
O3 absorption ~ 0 - 30
for aerosols: 0.01 - 5.0 Dt(l, z) ~ l-a
for clouds: 1-1000 a ~ 0cirrus ~ 1-5cumulonimbus ~ > 100
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For each layer, must specify Dt, wo, g:
2. Single scattering albedo, wo(l, z) = scatt./(scatt.+abs.)
range 0 - 1limits: pure scattering = 1.0
pure absorption = 0.0
for molecules, strongly l-dependent, depending onabsorber amount, esp. O3
for aerosols: sulfate ~ 0.99soot, organics ~ 0.8 or less, not well known but probably higher
at shorter l, esp. in UV
for clouds: typically 0.9999 or larger (vis and UV)
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34
For each layer, must specify Dt, wo, g:
3. Asymmetry factor, g(l, z) = first moment of phase function
range -1 to + 1pure back-scattering = -1isotropic or Rayleigh = 0pure forward scattering = +1
strongly dependent on particle sizefor aerosols:, typically 0.5-0.7for clouds, typically 0.7-0.9
Mie theory for spherical particles: can compute Dt, wo, g from knowledge of l, particle radius and complex index of refraction
1
1
)d(coscos)(2
1Pg
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SIMPLE2-STREAMMETHOD:3 Equations for each layer
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AEROSOLS
36
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37
Many different types of aerosols
• Size distributions• Composition (size-dependent)
Need to determine aerosol optical properties:
t(l) = optical depth
wo = single scattering albedoP(Q) = phase function or g = asymmetry factor
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Mie Scattering Theory
For spherical particles, given:
Complex index of refraction: n = m + ikSize parameter: a = 2pr / l
Can compute:
Extinction efficiency Qe(a, n) x pr2
Scattering efficiency Qs(a, n) x pr2
Phase function P(Q, a, n) or asymmetry factor g(a, n)
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Extinction Efficiency, Qext
10 100 1000 100000
1
2
3
4
5
300 nm
400 nm
Radius, nm
Qe
xt
n = 1.55 + 0.01i
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Phase function or Asymmetry factor, g
Asymmetry factor, g n = 1.5 + 0.01 i
0
0.2
0.4
0.6
0.8
1
200 300 400 500 600 700
Wavelength, nm
g
100 nm
300 nm
1000 nm
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Single Scattering Albedo = Qscatt/Qext
Single Scattering Albedo, o
n = 1.5 + 0.01 i
0
0.2
0.4
0.6
0.8
1
1.2
200 300 400 500 600 700
Wavelength, nm
o
100 nm
300 nm
1000 nm
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Aerosol size distributions
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Optical properties of aerosol ensembles
Total extinction coefficient =
Total scattering coefficient =
Average single scattering albedo =
Average asymmetry factor =
rrnrQrK ss d)(),()(0
2 ll
)(/)()( lll eso KK
0
2
0
2
d)(),(
d)(),(),(
)(
rrnrQr
rrnrQrrg
g
s
s
l
lll
rrnrQrK ee d)(),()(0
2 ll
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UV Actinic Flux Reduction Slower Photochemistry
44Madronich, Shetter, Halls, Lefer, AGU’07
300 320 340 360 380 4000
100000000000000
200000000000000
300000000000000
obs
tuv-clean
tuv-polluted
Wavelength, nm
Qu
anta
cm
-2 s
-1 n
m-1
18 March 16:55 LTsolar zenith angle = 65o
Mexico City
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Aerosol EffectsNO2 Photolysis Frequency
19N, April, noon, AOD = 1 at 380 nm
0
0.5
1
1.5
2
5.0E-03 1.0E-02 1.5E-02
JNO2, s-1
z, k
m
clean
purelyscattering
moderately absorbing(o=0.8)
Castro et al. 2001
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CLOUDS
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UNIFORM CLOUD LAYER
• Above cloud: - high radiation because of reflection
• Below cloud: - lower radiation because of attenuation by cloud
• Inside cloud: - complicated behavior– Top half: very high values (for high sun)– Bottom half: lower values
47
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EFFECT OF UNIFORM CLOUDS ON ACTINIC FLUX
340 nm, sza = 0 deg., cloud between 4 and 6 km
02468
10
0.E+00 4.E+14 8.E+14
Actinic flux, quanta cm-2 s-1
Alt
itu
de,
km
od = 100
od = 10
od = 0
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INSIDE CLOUDS:Photon Path Enhancements
Cumulonimbus, od=400
Mayer et al., 1998
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Broken Clouds
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SPECTRAL EFFECTS OF PARTIAL CLOUD COVER
Crafword et al., 2003
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PARTIAL CLOUD COVERBiomodal distributions
Crawford et al., 2003
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Independent Pixel Approximation
Cloud free:• So = direct sun• Do = diffuse light from sky• Go = total = So + Do
Completely covered by clouds:• S1 = direct sun (probably very small)• D1 = diffuse light from base of cloud• G1 = total = S1 + D1
Mix: Clouds cover a fraction c of the sky• If sun is not blocked: GNB = So + cD1 + (1-c)Do • If sun is blocked: GB = S1 + cD1 + (1-c)Do
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Photochemistry Inside Liquid Particles
clouds
aerosol
Mayer and Madronich, 2004
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Radiative Forcing of
Climate
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Shortwave and Longwave Radiation
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Energy Balance
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Infrared Absorbers
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Very Structured Spectra
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Radiative Forcing
IPCC, 2007
Incoming solar ~340 W m-2
1827 – Fourier recognizes atmospheric heat trapping
1860 – Tyndall measures infrared spectra
1896 – Arrhenius estimates doubling of CO2
would increase global temperatures by 5-6 oC
Changes since 1750:long-lived gases ~ 3 W m-2
ozone ~ 0.4 W m-2
aerosols and clouds ~ -1 W m-2
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Some Climate Model Problems
11 models compared
All predict 20th century climate
well, but for different reasons
Trade off between
- aerosol forcing
- climate sensitivity
Climate sensitivity = DT for doubling of CO2
61Kiehl, 2007
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Biological Effectsof
Ultraviolet Radiation
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Non-melanoma Skin Cancers
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Moles and Melanoma
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Melanoma Warning SignsAsymmetry, Border, Color, Diameter (ABCD)
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Damage to Eyes
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ACTION SPECTRUM DETERMINATION
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Ocular damage action spectra (normalized at 300 nm)
0.0001
0.001
0.01
0.1
1
10
100
280 300 320 340 360 380
Wavelength, nm
Se
ns
itiv
ity
cataract pig (Oriowo)
cataract rat (Merriam)
cataract rabbit (Pitts)
conjunctiva human (Pitts)
cornea rabbit (Pitts)
cornea primate (Pitts)
cornea human (Pitts)
uvitis rabbit (Pitts)
ave-Pitts only
ave-all ocular
erythema human (CIE)
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SPECTRALLY INTEGRATED RADIATION
Radiometry
Signal (W m-2) = l E(l) R(l) dl
Biological effects
Dose rate (W m-2) = l E(l) B(l) dl
Photo-dissociation of atmospheric chemicals
Photolysis frequency (s-1) = l F(l) s(l) f(l) dl
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Changes in surface irradiance, for 1% O3 change
Near 300 DU
Solid: Absolute
(mW m-2 nm-1)
Dotted: Relative
(percent)
Heavy: sza = 0o
Light: sza = 70o
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Observed dependenceof UV on O3 changes (clear sky)
Madronich et al. 1998
For erythemal (sunburning) radiation
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Global Climatology of UVR from Satellites
Total Ozone Mapping Spectrometer (TOMS):– Nimbus 7 (1 Nov 1978 – 31 Dec 1992)– Meteor 3 (22 Aug 1991 – 11 Dec 1994)– Earth Probe (2 Jul 1996 – 30 Jun 2000)
Data (Level 3/Version 7):– O3 by UV-B wavelength pairs– Cloud reflectivity at 380 nm– 1.25o lon x 1.00o lat
Model:– TUV look up tables for erythemal irradiance, as functions of
sza, O3, surface elevation– Calculate for each location, 15 min of each half day, each
month, each year
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UVERY climatology, 1979 to 2000 - Clear skies
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UVERY climatology, 1979 to 2000 - All skies
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UVERY change, 1980’s to 1990’sClear sky (ozone changes only)
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Cloud factor % changes, 1980’s to 1990’s
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UVERY % change, 1980’s to 1990’sAll sky conditions (ozone and cloud changes)