OOP&M - theory lectures1 OOP&M – the sixth day “… there must be a secret out there …” - Spok -
Web page: ...harnik/GCirc/lectures1-2.pdf · John Marshall and Alan Plumb, (2007), “Atmosphere,...
Transcript of Web page: ...harnik/GCirc/lectures1-2.pdf · John Marshall and Alan Plumb, (2007), “Atmosphere,...
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References:
Main text:•
Geoffrey Vallis
(2006) “Atmospheric and Oceanic Fluid Dynamics.”
Cambridge press. Part III-
Large
scale atmospheric circulation (chapters 11-12). Parts rely on the theory developed in parts I, II.
Other texts and supplemental reading (partial list):•
Richard Lindzen
(1990) “Dynamics in atmospheric physics.”
Cambridge press. In particular the
chapter on the Hadley cell (7). Chapter 5 on the observed circulation is also good. •
Holton, (1992, 2004) “An introduction to dynamic meteorology.”
Elsevier, Academic Press. Chapter
on the general circulation (10).•
Dennis Hartmann (1994), “Global Physical Climatology”.
•
John Marshall and Alan Plumb, (2007), “Atmosphere, Ocean and Climate dynamics”. An introductory level text book with nice rotating tank experiments and a good basic physical understanding.
•
Tapio
Schneider (2006) The general circulation of the atmosphere, Annu. Rev. Earth. Planet. Sci. A review article which can be found online at http://www.gps.caltech.edu/~tapio/pubs.html
•
Edward N. Lorenz (1967) “The nature and Theory of the general circulation of the atmosphere.”
WMO monograph 218. Includes a historical overview of general circulation theories.
•
Isaac Held (2000) The general circulation of the atmosphere. Woodshole
summer school class notes, found at http://www.gfdl.noaa.gov/~ih/. General circulation theory.
•
Peixoto
and Oort
(1992) “Physics of Climate.”
AIP. Introduction to the equations and general circulation “observations”.
Web page: http://geophysics.tau.ac.il/personal/nili/GCirc/GCirc-course.htm
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Thermal wind balance
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Palmen
and Newton (1969)
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Janu
ary
300mb surfaceJu
ly
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Midlatitude
weather systems
NOAA NCEP-NCAR CDAS-1 DAILY300 mb
height (m) and winds (m/s) 1 Apr 1997
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. m/sec :יחידות. המרידיונאלית ושנתי של המהירות זונאלי ממוצע. מהירות חיובית היא זרימה צפונה ושלילית זרימה דרומה : זכרו
) ושנתי של מהירות הלחץ האנכית זונאלי ממוצעdtdp
10-4mb/sec .
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The Zonally Averaged vertical- meridional Circulation
The annually-averaged atmospheric circulation in the latitude pressure plane (the meridional plan). The arrows depict the direction of air
movement in the meridional plane. The contour interval is 2x10
10 Kg/sec -
this is the amount of mass that is circulating between every two
contours. The total amount of mass circulating around each "cell" is given by the largest value in that cell. Data based on the NCEP-NCAR
reanalysis project 1958-1998.
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. חסר יחידות. ושנתי של הלחות הסגוליתזונאלי ממוצע.חסר יחידות . ושנתי של הלחות הסגולית ברוויה זונאלי ממוצע
: %.יחידות. ושנתי של הלחות היחסיתזונאלי ממוצע
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Climate Zones according to Koeppen
•For more information about this map see:
•http://www.blueplanetbiomes.org/climate.htm
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I assume you already know that :
Energy balance -
what comes in must go out
Earth is heated by short wave (energetic) solar radiation
and cooled by emitting less energetic,
long wave infra-red (IR) radiation.
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The incoming solar radiation is partly reflected back to space (30%), partly absorbed by the atmosphere, and partly absorbed by the earth (50%).
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•Latent heat –
water cools the surface when it evaporates into the air, and releases heat when it condenses into cloud and rain drops
•Sensible heat –
hot buoyant air convection
•IR radiation
The earth’s surface, which absorbs much of the solar radiation, emits heat in 3 ways:
on which we will concentrate next…
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The atmosphere is a mixture of molecular Nitrogen and Oxygen, with a bit of Argon, and trace amounts of other gases, like CO2. Water varies between ~0.4% in very dry air, to ~4% in the tropics.
What happens when IR radiation hits the air molecules?
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That depends on the type of molecule and radiation
Molecules have energy, stored in the bonds between atoms, and in
the relative motions between the different molecule atoms.
When radiation hits a molecule, it will pass its energy on to the molecule, if the molecule can “contain”
this energy.
Thus, each mode of energy absorption occurs at a specific narrow
band of the solar spectrum.
Radiation energy spectrum
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Energetic UV radiation can break apart the molecules.
For example: breakup of O2
, to form O3
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Visible light does not interact with air molecules. Our eyes developed to make use of this, to see things on earth.
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IR radiation gets absorbed by exciting rotational and vibrational
modes of specific
molecules
Absorption of electromagnetic radiation requires an electric dipole.
Electric dipoles require some asymmetry in the molecule structure.
O2
, N2
don’t interact with IR radiation.
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Wavelength (microns)
% A
bsor
ptio
n
H2
O absorption spectrum
H2
O molecules have a triangular structure, with a dipole.
IR is absorbed by exciting vibrational
and rotational
energy.
vibrationrotation
Vibration- rotation
bands continuum
Used in microwave ovens
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CO2
and H2
O
absorption spectrum
CO2
molecules have a linear symmetric structure, with no dipole, but when they vibrate, the symmetry breaks, a dipole forms and IR can be absorbed
15 m
Wavelength (microns)
% A
bsor
ptio
n
Some of the CO2 vibration bands lie in the water vapor “windows”
4.3 m
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Most important are the absorption peaks which sit on the Earth’s peak emission spectrum:
H2
O -
6.3m
H2
O > 12m
CO2
– 15m
O3
– 9.6m
Other gases also absorb IR: O3
, CH4
, NO
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The IR radiation which is absorbed in the air molecules is emitted back out in all directions (including the surface).
Part of the energy absorbed causes the molecules to move faster
temperature rises.
When temperature rises, more radiation is emitted (black body)
Temperature will rise until equilibrium is reached.
sun
earth
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Equations…
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ground
The terrestrial IR radiation gets gradually absorbed as it propagates upwards in the atmosphere.
The IR emitted from each layer, also gets gradually absorbed in the layers above and below.
The full problem consists of summing up the contributions and effects of all layers.
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Effect of Atmospheric Absorption: 1 sheet
σΤg4 = S0
4(1-α)
w/o absorption w. absorption
= S04(1-α)σΤa
4
σΤg4 = S0
4(1-α) + σΤa4
ground
α
(1-α)
atmosphere
S04
σΤg4
absorption of solar emission of IR
S04
S04
ground
α
atmosphere
σΤg4IR
absorbinglayer
H=σΤa4
H(1-α)
S04
S04
S04
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Effect of Atmospheric Absorption: 1 sheet
w/o absorption w. absorption
= S04(1-α)σΤa
4
σΤg4 = S0
4(1-α) + σΤa4
σΤg4 = S0
2(1-α)
Τg =S02σ(1-α)
4
σΤg4 = S0
4(1-α)
Τg = S04σ(1-α)
4
W/O absorption: Tg
=255 K or -18°C
W. absorption Tg
=303.5 K or +30.5°C
The Greenhouse
Effect
= 239 Wm-2
Too warm
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2 layersN layersSurface and surface air temperature
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ground
σΤg4
H=σΤa4
H
Since radiation makes the surface hotter than the air just above it, the surface looses heat not only through radiation, but also through latent and sensible heat transports (both upwards and polewards).
These fluxes do not depend so strongly on temperature –
a linear,
rather than “to the 4th” dependence on T:
σΤg4 = S0
4(1-α) + σΤa4AΤg
+B+
This yields colder Tg
than with pure radiative surface cooling
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Radiative convective equilibrium…Manabe
and Strickler, 1964
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Clouds complicate the picture:Thin high cirrus clouds reflect little solar radiation, and absorb IR efficiently. They then emit IR at a cold temperature (air is colder higher up)
net warming
Low thick clouds reflect solar radiation efficiently. They absorb IR, but they emit at a relatively warm temperature (near the ground)
net cooling
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Overall, we get a surface temperature of Tg
=(390/σ)1/4=288°K=15°C
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LW Cooling SW Heating
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Incoming Solar (Shortwave) at TOA
December March
June September
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Daily mean incoming solar radiation at top of the atmosphere (W/m2)
Latit
ude
Time of yearBased on ERBE data
declination
Length of day
Eccentricity – global monthly
mean TOA SW
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Reflected Solar at TOA
December March
June September
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Planetary Albedo
December March
June September
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Net Shortwave (Solar) Radiation
December March
June September
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Net daily solar radiation at surface
Daily incoming radiation at top of atmosphere during December –
ozone
heating distribution
W
W
W
W
C C
C
C
C
C
Latitude-height zonal mean temperature structure
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Outgoing Longwave (IR) at TOA
December March
June September
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Net Incoming Radiation (LW and SW)
December March
June September
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Outgoing longwave
radiation (OLR) Net Shortwave (Solar) Radiation
Net incoming Radiation (SW-LW)
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Latitudinal Radiation Imbalance
adapted from Trenberth
and
Caron (2001)
PW=1015
W
Totalheat
transport
Atmosphericheat
transport
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Meridional heat transport
Trenberth
and Caron (2001)
PW=1015
W