Heat transport Water cycle Atmospheric circulation

1. Processes forcing the climatic conditions • Heat transport • Water cycle • Atmospheric circulation

2. Radiation There are four main processes of energy transport in the atmosphere: radiation, molecular conduction turbulent conduction latent heat sensible heat

3. Thermal Energy • All matter is composed of atoms or molecules, which are in constant motion • Molecular or atomic motion = “thermal energy” • Heating atoms causes them to move faster, which represents an increase in thermal energy. • Temperature is a measure of thermal energy.

4. Radiation is the way of energy transport by electromagnetic wave moving with the speed of light. It does not demand any medium. Energy is transmitted in portions called kwantums. wavelength crest through wavelength × frequency = speed of light

5. Energy of a wave Energy is proportional to frequency, and inversely proportional to wavelength E = h  = h (c/ ) whereh = Planck’s constant In other words, waves with shorter wavelengths (or higher frequency) have higher energy

6. Each body with temperature higher than 0K (-273,13ºC) emits radiation to space, ie. emits an electromagnetic wave moving with the speed of light differing in wavelength, frequency and amplitude.

7. All bodies, withtemperaturegreaterthanabsolute 0, emitradiation. Therateatwhichsomethingradiates and absorbs energy dependsstrongly on itssurfacecharacteristics, such as color, texture, moisture and temperature. Thereis a group of bodiescalledblackbodies. Therateatwhichtheyradiate energy dependsonly on theirtemperature. Theyareperfect absorber of radiation (absorballradiationthatstrikesthem) and a perfectemitter (emitthemaximumradiationpossibleattheirtemperature).

8. Blackbody Radiation Law of Planck Blackbody radiation—radiation emitted by a body that at all wavelengthsemits (or absorbs) energy in the amount described by law of Planck.

9. Basic Laws of Radiation • All objects emit radiant energy.

10. Basic Laws of Radiation • All objects emit radiant energy. • Hotter objects emit more energy than colder objects.

11. Basic Laws of Radiation • All objects emit radiant energy. • Hotter objects emit more energy than colder objects. The amount of energy radiated is proportional to the temperature of the object raised to the fourth power.

12. Basic Laws of Radiation • All objects emit radiant energy. • Hotter objects emit more energy than colder objects. The amount of energy radiated is proportional to the temperature of the object raised to the fourth power. •  This is the Stefan Boltzmann Law • E =  T4 • E = flux of energy (W/m2) • T = temperature (K) •  = 5.67 x 10-8 W/m2K4 (a constant)

13. Basic Laws of Radiation • All objects emit radiant energy. • Hotter objects emit more energy than colder objects (per unit area). The amount of energy radiated is proportional to the temperature of the object. • The hotter the object, the shorter the wavelength () of emitted energy.

14. Basic Laws of Radiation • All objects emit radiant energy. • Hotter objects emit more energy than colder objects (per unit area). The amount of energy radiated is proportional to the temperature of the object. • The hotter the object, the shorter the wavelength () of emitted energy. • This is Wien’s Law • max  3000 m • T(K)

15. Stefan-Boltzmann law E =  T4 E = flux of energy (W/m2) T = temperature (K)  = 5.67 x 10-8 W/m2K4 (a constant) Wien’s law max  3000 m T(K)

16. The amount of energy emitted by the black body at wavelength  is depends only on the object temperature and is described by Planck's law: k Bolzmann's constant (k=1,38·10-23J/K) T temperature in Kelvin scale c – speed of light (3,0·108m/s), h - Planck's constant (h=6,63·10-34J·s),

17. solar spectrum Earth's spectrum

18. We can use these equations to calculate properties of energy radiating from the Sun and the Earth. 6,000 K 300 K

20. Wien’s law: max  3000 m T(K)

22. Stefan-Boltzmann law:E =  T4

23. energy Hotter objects emit more energy than colder objects E=σT4 Sun Earth 0.01 0.1 1 10 100 1000 wavelength

24. Hotter objects emit at shorter wavelengths. max = 3000/T energy Sun Earth 0.01 0.1 1 10 100 1000 wavelength

25. Outgoing Longwave Radiation (OLR) Anomalies Drier-than-average conditions (orange/red shading) Wetter-than-average conditions (blue shading) From October – December 2011, variability in OLR anomalies (focused mostly over the Indian Ocean and Maritime Continent) was associated with the MJO. Since April 2010, negative OLR anomalies have been observed near the Maritime Continent and positive OLR anomalies have prevailed over the western and central Pacific. Recently, eastward propagation of negative OLR anomalies is evident in association with the MJO. Time Climate Prediction Center / NCEP Longitude

28. visible light UV infrared radiation wavelength

29. Intensity of solar radiation at the upper boundary of the atmosphere is called solar constant and amounts on average 1353 W/m2. Solar constant is not perfectly constant. The elliptical path of the Earth around the Sun brings the Earth closer to the Sun in January (147 mln km in aphelium) than in July (152 mln km in perihelium). From this reason the changes in solar constant during the year are about 3.5%. Since 1978 the remote sensing has been measured. It appears that the solar constant is also changing with solar activity. These changes did not exceed the level of 0.08% during the 30 years of measurements. In very long time scale (thousands of years) the orbital parameters of the Earth path around the Sun cause some changes in solar constant. The intensity of solar radiation is also changing in the long history of the Earth. 3.5 billions of years ago the Sun emitted only 70 % of radiation it is emitting today.

30. Solar radiation is emitted in each direction equally. Because the distance from the Sun to the Earth is really huge than the radiation reaching the surface is parallel. The amount of energy reaching the earth surface in the time unit is called intensity of direct solar radiation. Radiation that strikes a surface at an angle is spread over a larger area than the radiation that strikes the surface directly.

31. All objects with temperature above absolute zero emit radiation. • The higher the object temperature, the greater the amount of radiation emitted per unit surface area and the shorter the wavelength of maximum emission. • The Earth absorbs solar radiation only during the daylight hours; however, it emits infrared radiation continuously, both during day and at night. • The Earth’s surface behaves as a black body, making it a much better absorber and emitter of radiation than is the atmosphere

32. reflection absorption and emission scattering

33. In the atmosphere the radiation can be: • scattered, • absorbed • reflected. When sunlight strikes a very small objects such as air molecules and dust particles the light itself is deflected in all directions – forward, sideward and backward. It is called scattering. Scattering on a tiny particles was firstly described by English scientist lord Rayleigh (1842-1919) and is called a Rayleigh scattering. iλ - intensity of scatttered radiation of wavelenght λ, Iλ - intensity of direct radiation of wavelenght λ, k – coefficient of scattering.

34. Absorption During the absorption process, the infrared radiation is converted into internal energy. Gases in our atmosphere are selective absorbers. Ozone, for example, absorbs UV radiation, especially at wavelengths between 0.2 and 0.3 μm, and an infrared radiation at 9.6 V μm. Molecular oxygen absorb UV radiation below 0.2 μm. Water vapor and carbon dioxide absorb energy in the infrared wavelengths.

35. ABSORPTION in the ATMOSPHERE During the absorption process, the absorbed radiation is converted into internal energy. Gases in our atmosphere are selective absorbers. Ozone, for example, absorbs UV radiation, especially at wavelengths between 0.2 and 0.3 μm, and an infrared radiation at 9.6 V μm. Molecular oxygen absorb UV radiation below 0.2 μm. Water vapor and carbon dioxide absorb energy in the infrared wavelengths. visible infrared

36. Absorption of radiation by gases in the atmosphere

37. White or shiny objects reflect sunlight from their surface.An object that reflects a great deal of radiation of sunlights absorbs (and emits) very little. The percent of radiation returning from the surface compared to the amount of radiation stiking it is called the albedo of the surface.

39. Earth surface radiation balance income outcome direct radiation scattered radiation direct radiation falling on flat surface total radisation falling on flat surface radiation emitted by the Earth solar radiation absorbed by the Earth surface radiation transmitted downward efective radiation of the Earth

40. Daily course of temperature and balance of radiation

41. The Earth annual radiation balance and temperature course

46. Influence of ground cover type on heat balance net radiation input latent heat used for evapotranspiration sensible heat used for warming of the air exchange with the ground

47. Types of heat balance