1. (2) Radiation Laws 1 Physics of the Atmosphere II Atmo II 31

2. Angle and Solid Angle Atmo II 32 Radian (rad) is the standard unit for angular measures. In a circle (with radius r) 1 rad corresponds to an arc length = r. The whole circumference is therefore 2 π rad = 6.2832 rad. Steradian (sr) is the standard (SI) unit for solid angles. On a sphere (with radius r) 1 sr corresponds to an area = r 2. The whole surface area is therefore 4 π sr = 12.5664 sr. www.greier-greiner.at Wiki

3. Solid Angles on Earth Atmo II 33 Solid angles of different areas on Earth (Zimbabwe, Algeria + Libya, Switzerland – or Austria) Wiki

4. Radiation Units Atmo II 34 Try not to be confused ! Radiant energy: Energy [J] Radiant flux: Energy per time [J s –1 ] = [W] (power) Radiant flux density = Irradiance: Energy per time per area [J s –1 m –2 ] = [W m –2 ] Radiance: Energy per time per area per solid angle [W m –2 sr –1 ] Spectral radiance Spectral radiance with respect to wavelength [W m –2 sr –1 m –1 ] = [W m –3 sr –1 ] or Spectral radiance with respect to frequency: [W m –2 sr –1 Hz –1 ]

5. Strahlungsgrößen Vorsicht – Verwirrungsgefahr ! Strahlungsenergie: Energie [J] Strahlungsfluss: Energie pro Zeit [J s –1 ] = [W] (also eine Leistung) Strahlungsflussdichte = Irradianz: Energie pro Zeit pro Fläche [J s –1 m –2 ] = [W m –2 ] Strahldichte = Radianz: Energie pro Zeit pro Fläche pro Raumwinkel [W m –2 sr –1 ] Spektrale Dichte der Strahldichte: Strahldichte bezogen auf die Wellenlänge [W m –2 sr –1 m –1 ] = [W m –3 sr –1 ] oder Strahldichte bezogen auf die Frequenz [W m –2 sr –1 Hz –1 ] Atmo II 35

6. Planck’s Law According to Planck’s Law (Max Planck, 1900) the energy emitted by a black body (un-polarized radiation) per time, area, solid angle and wave length λ equals: c 0 = Speed of light (in vacuum) = 299 792 458 m s –1 h = Planck constant = 6.626 069 57·10 –34 Js k B = Boltzmann constant = 1.380 6488·10 –23 J K -1 According to our last slides this has to be – right: Spectral radiance with respect to wavelength [W m –2 sr –1 m –1 ] Atmo II 36

7. Planck’s Law Planck’s Law (last slide) refers to un-polarized radiation per solid angle. In case of linear polarization we would just get half of it. If you should miss a factor π – this comes be integrating over the half space. Planck‘s law often comes in frequency formulation: Atmo II 37

8. Planck–Function Black-Body Radiation (Planck Functions) for different temperatures (wikimedia). Note the large dynamic range due to the extremely strong wavelength dependence. Atmo II 38

9. Planck Functions in double logarithmic representation (wikimedia). Note that black bodies with higher temperatures emit more energy at all wavelengths. Planck–Function Atmo II 39

10. Planck Function for the temperature of our Sun (yes, the sun can indeed be regarded as a black body !) (Meteorology Today, C. D. Ahrens). 44 % of the total energy is emitted in the visible part of the spectrum. But also in the thermal infrared the suns emits way more energy (per m 2 ) than the Earth. Planck–Function – Sun Atmo II 40

11. But how about pictures like this? (LabSpace). These are scaled representations, showing λ B λ on the y-axis – and the solar radiation intercepted by the Earth (and not emitted by the Sun). Planck–Functions? Atmo II 41

12. Integrating Planck’s Law If we want just to know the total power emitted per square meter, we need to integrate the Planck law twice – over the half space and over all wavelengths. The integral over the half space gives: Atmo II 42 Effective area: K. N. Liou Black body radiation is isotropic (independent of the direction):

13. Stefan–Boltzmann Law The integral over all wavelengths gives: Atmo II 43 But this is nothing else than:

14. The famous Stefan–Boltzmann Law (after Josef Stefan and Ludwig Boltzmann): σ = Stefan–Boltzmann constant σ = 5.670 373 · 10 –8 W m –2 K –4 Atmo II 44 Stefan–Boltzmann Law The Stefan–Boltzmann constant is therefore related to even more fundamental constants: (Please try it without calculator)

15. Solar Constant How much solar radiation reaches the Earth? Looking at a point-source, and considering energy conservation, we see that concentric spheres must receive the same energy (blackboard). Die radiant flux density (irradiance), at the mean distance Earth – Sun (= Astronomical Unit – AU) per square meter is termed Solar Constant and has (probably) the value: where the Solar Radius R Sun = 695 990 km (about. 0.7 Mio km), and the Astronomical Unit r S–E = 149 597 871 km (about 150 Mio. km). but S 0 is not constant. The brightness temperature of the Sun is 5776 K. Atmo II 45

16. Measuring the Solar Constant Atmo II 46 Total Solar Irradiance (TSI) measurements – composite of different satellite measurements (World Radiation Center).

17. Measuring the Solar Constant Atmo II 47 TSI measurements – original measurements (source: WRC). Systematic difference ~ anthropogenic radiative forcing. Trend estimation impossible without data overlap.

18. Changing Solar Constant Atmo II 48 Changes in the total solar irradiance due to the ~11 year solar cycle (about 1 W/m 2 or 1 ‰) are comparatively small (NASA GISS). Note the pronounced latest minimum.

19. Changing Solar UV Radiation Atmo II 49 Changes in the UV part of the spectrum are much more distinct (NASA).

20. Solar Insolation In general, a square meter on Earth will not receive the full solar constant, since the solar radiation will not hit at right angle (keywords – seasons, night). With the zenith angle of the sun, θ, we get S = S 0 cosθ (Lambert’s Cosine Law). And not all the radiation will reach the ground. W & K Atmo II 50

21. Solar Insolation Daily mean solar insolation as a function of latitude and day of year in units of Wm −2 based on a solar constant of 1366 Wm −2. The shaded areas denote zero insolation. The position of vernal equinox (VE), summer solstice (SS), autumnal equinox (AE), and winter solstice (WS) are indicated with solid vertical lines. Solar declination is shown with a dashed line (K. N. Liou). Atmo II 51

22. Solar Radiation at the Surface At the “top of the atmosphere“ the solar irradiance is still close to that of a black body (R.A. Rhode). Even under “clear sky” conditions a part of the incoming radiation will be scattered and absorbed (the latter – about 20 % mainly due to Ozone and Water Vapor). Atmo II 52

23. Albedo Albedo is the percentage of the solar radiation, which is directly reflected. Die Albedo depends on the surface properties. The Albedo is particularly high for (dense) clouds and (fresh) snow. The Earth as a whole reflects 31% of the incoming solar radiation (A = 0.31). The Earth-surface therefore only absorbs about 50 % of the solar radiation. Surface Albedo Clouds 45-90 % Fresh snow (3)75-95 % Glaciers20-45 % Sea Ice30-40 % Rock, soil (2)10-40 % Forests (1) 5-20 % Water 5-10 % Planetary Albedo 31% Atmo II 53

24. Albedo Annual mean of the top of the atmosphere (toa) Albedo (Raschke & Ohmura*) Atmo II 54

25. Net-Short-Wave Radiation = SW down – SW up at the Earth‘s surface. Shortwave-Radiation Atmo II 55

26. Annual mean toa Net Shortwave Radiation (Raschke & Ohmura*) Shortwave-Radiation Atmo II 56