Solar and Terrestrial Radiation
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1 Solar and Terrestrial Radiation I Heat and Temperature A. 1. A form of. 2. The total of all the atoms and molecules of a substance 3. Heat always moves from a temperature body to a temperature body. B. 1. The of the individual atoms or molecules in a substance 2. Addition of heat energy causes atoms to and removal causes atoms to down. 3. The total amount of heat of a substance depends upon its. For example, a substance can have a high temperature and small amount of heat while another may contain a large amount of heat and have a low temperature. 4. a. A unit for measuring the quantity of heat when an object is heated or cools off. b. Defined as the quantity of heat needed to raise the temperature of one gram of 5. a. Defined as the quantity of heat needed to raise the temperature of by one degree Celsius. b. The the specific heat of a substance, the the amount of heat needed to raise its temperature. i. Water has the specific heat of all natural substances (1.0 cal/g C) o ii By comparison the only 0.20 calories are required to heat one gram of the rock basalt one degree Celsius (basalt has a specific heat of ) MET 102: Professor Vorwald Solar and Terrestrial Radiation Page 1 of 8
2 6 Heat Loss or Gain can be expressed by the following equation. Q = m T C p Where: Q = total heat lost or gained; m = mass in grams; T = change in temperature of the substance; C = specific heat of the substance p C. Methods of Heat Transfer 1. a. The transfer of heat through electron and molecular from one molecule to another. b. Conduction is important only between Earth s and the air immediately in with the surface. c. As a means of heat transfer for the atmosphere as a whole, conduction is the least significant and can be disregarded when considering most meteorological phenomena. 2. a. Heat transfer that involves movement or circulation of a substance. b. Takes place in where the material is able to flow. c. i. Takes place when the fluid near the bottom is heated and becomes dense. ii. It rises, cools near the top and continues to turn over. iii. Air moves vertical in the atmosphere. Less dense air rises and transports heat to greater heights. 3. a. The heat-transfer mechanism by which energy reaches Earth. b. Doesn t require a medium in which to travel and can pass through the space. c. The Sun emits and along with the rest of electromagnetic spectrum of radiation. II Insolation (Incoming Solar Radiation) A. : 1. Travels out in all directions from the Sun and does travels through the of space. 2. Heat transfer mechanism for energy. MET 102: Professor Vorwald Solar and Terrestrial Radiation Page 2 of 8
3 3. The Sun emits wavelengths a. Most is concentrated in the (43%) b. Infrared to visible represents 49% c. represents 7%. 2. Laws of Radiation a. objects, at whatever temperature, emit radiant energy. b. Hotter objects radiate energy per unit area than colder objects c. The hotter the radiating body, the the wavelength of maximum radiation. d. Objects that are good absorbers of radiation are also. i. A is considered a perfect absorber and emitter. Earth s surface approaches being a blackbody because it absorbs and radiates with nearly100percent efficiency. ii. Surface characteristics affect absorption and emission. (1) Color: (2) Reflectivity (3) Texture (4) Land vs. Water B. Intensity of Insolation 1. This is the at which solar energy is received by a given of Earth s surface per unit of (usually calories/second/square centimeter). 2. : The angle at which the Sun s rays strike Earth s surface. a. Rays strike the surface at right angles. They are. b. As the angle decreases, the rays become direct and insolation is spread out over a area. c. Therefore, the more direct the rays striking Earth s surface, the the intensity of insolation. MET 102: Professor Vorwald Solar and Terrestrial Radiation Page 3 of 8
4 3. Factors Affecting the Angle of Insolation a. Latitude: b. Time of Day: c. Season: III The Seasons A. Observations 1. Change in length of. 2. Change in the sun s across the sky a) Change in and positions b) Change in altitude (solar noon or high noon) i) Change in angle of of Sun s rays with Earth s surface ii) Change in of atmosphere through which the Sun s rays pass B. Causes of changing the Sun s noontime altitude and diurnal path throughout the year 1. Earth s to the Sun continually changes as it around the Sun. 2. Earth s axis is inclined from a line perpendicular to the plane of it s orbit 3. of Earth s axis: A. Earth s axis always points in the in space. B. The orientation of the axis is at any position in its orbit always to any other position. MET 102: Professor Vorwald Solar and Terrestrial Radiation Page 4 of 8
5 C. Solstices and Equinoxes 1. Summer Solstice (Northern Hemisphere): a) Northern axis tilts the Sun b) Sun s direct rays at latitude 2. Winter Solstice (Northern Hemisphere) a) Northern axis tilts from the Sun b) Sun s direct rays at latitude 3. Equinoxes (Autumnal and Spring which is also called the vernal equinox) a) between the solstices b) Sun s direct rays. 4. Latitude of the Sun s Vertical Rays for Various Dates of the Year o Noon Alt. of Sun = 90 minus the distance in degrees between observer s latitude and the latitude receiving vertical rays for that date. IV The Atmosphere and Insolation A. What Happens to Insolation? 1. Scattering a. Insolation is redirected by gases and dust particles ( ) in the atmosphere b. Produces light. i. Degree of scattering depends on of particles or gas molecules ii. iii. When light is scattered by very small particles, primarily gas molecules, it is distributed in all directions but most is scattered in the forward direction. Light lost to space is said to be. The blue color of the sky: (1) Gas particles more readily scatter shorter wavelengths (blue and violet). (2) During midday blue light is seen because it is most readily scattered. (3) When the Sun is lower light travels a longer path. (4) color seen because most blue and violet is scattered before reaching the observer. MET 102: Professor Vorwald Solar and Terrestrial Radiation Page 5 of 8
6 2. Reflection a. Approx. 30% of insolation is reflected back into space by the outer atmosphere. b. : The fraction reflected by a surface. i. Varies with characteristics of the surface. ii Varies with weather conditions and time of day and year. B. Heating the Atmosphere 1. are the most effective absorbers of radiation and heat the atmosphere 2. The atmosphere is nearly to incoming solar radiation. Direct solar energy is not an effective heater of Earth s Atmosphere. 3. The only significant absorbers of insolation are: a. b. : High energy, shortwave radiation c. : High energy, shortwave radiation in the Stratosphere 4. The atmosphere is a relatively efficient absorber of long-wave (infrared) radiation. C. Terrestrial Radiation and Heating of the Atmosphere 1. Emitted in wavelengths 2. range terrestrial radiation heats the atmosphere. As a result, the atmosphere heats from the ground up. o 3. Normal Lapse Rate: 6.5 C temperature decrease per 1000 meters of altitude. The farther from the source of heat (the ground), the cooler it gets 4. and are principal absorbing gases, accounting for warmer temperatures in the lower troposphere. MET 102: Professor Vorwald Solar and Terrestrial Radiation Page 6 of 8
7 D. (Referred to by some scientists as the Atmosphere Effect) 1. The transmission of shortwave solar radiation by the atmosphere coupled with the selective of longer-wave terrestrial radiation, especially by water vapor and carbon dioxide, resulting in warming of the atmosphere. 2. Effects of cloud cover: a) absorbed terrestrial radiation to the surface. b) Clear nights vs cloudy nights c) Low cloud cover in desert regions results in daily temperature ranges. V Earth s Heat Budget A. Annual and Daily Balance of Incoming and Outgoing Radiation 1. Surplus a. Insolation is than terrestrial radiation. b. Temperatures. c. The greater the surplus the the rate of temperature increase. 2. Deficit a.. Insolation is terrestrial radiation. than b. Temperatures. c. The greater deficit, the the rate of temperature decrease. 3 Time-Lag between Maximum Insolation and Maximum Temp. and between Minimum Insolation and Minimum Insolation MET 102: Professor Vorwald Solar and Terrestrial Radiation Page 7 of 8
8 B. Latitudinal Heat Balance (Heat Equator) 1. Heat Equator: A line connecting the highest average temperatures by longitude for a given time period. 2. Observations: MET 102: Professor Vorwald Solar and Terrestrial Radiation Page 8 of 8
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