Radiation
Radiation

Radiation

Radiation

introduction

Radiation Heat radiation (as opposed to particle radiation) is the transfer of internal energy in the form of electromagnetic waves. For most bodies on the Earth, this radiation lies in the infrared region of the electromagnetic spectrum.

One of the first to recognize that heat radiation is related to light was the English astronomer William Herschel, who noticed in 1800 that if a thermometer was moved from one end of a prism produced spectrum to the other, the highest temperatures would register below the red band, where no light was visible. Because of this position, this form of radiation is called infrared (infra being the Latin word for below or within). Sometimes this kind of radiation is called “heat waves” but this is a misnomer. Recall that heat is the transfer of internal energy from one region to another. As all forms of electromagnetic radiation transfer internal energy, they could all be called “heat waves”.

stefan-boltzmann law

Hot objects are “brighter” than cold objects. Dark objects are lose and gain heat faster than light objects.

The Stefan-Boltzmann law relates the heat flow rate emitted or absorbed from an object to its temperature (and surface area and darkness). It was empirically derived by the Austrian physicist Joseph Stefan in 1879 and theoretically derived by the Austrian physicist Ludwig Boltzmann in 1884. It is now derived mathematically from Planck’s law.

Φ = εσA(T4 − T04)

where…

Φ = (phi) net heat flow rate [W] emitted (+) or absorbed (−)
ε = (epsilon) emissivity, a dimensionless (unitless) measure of a material’s effective ability to emit or absorb thermal radiation from its surface; ranges from 0 (none) to 1 (maximal)
σ = (sigma) Stefan constant, 5.670 × 10−8 W/m2K4
A = surface area [m2] of the object emitting or absorbing thermal radiation
T = absolute temperature [K] of the object emitting or absorbing thermal radiation
T0 = absolute temperature [K] of the environment

Connect Stefan-Boltzmann law to Planck’s law.

σ =
5k4  = π2k4
15h3c2 60ℏ3c2
σ = 5(1.38× 10−23 J/K)4
15(6.63 × 10−34 Js)3(3.00 × 108 m/s)2
σ = 5.67 × 10−8 W/m2K4

Dark colors absorb more radiant energy than do light colors. The burns on this woman’s skin mimic the pattern on her blouse. She was exposed to a monstrous dose of electromagnetic radiation from a nuclear blast. (Source: NARA)

Disconnected thoughts that aren’t quotes.

  • blackbody radiation, cavity radiator, the sun is a blackbody
  • For humans, the emissivity in the infrared region is independent of the color of the skin and is very nearly equal to 1, indicating that the skin is almost a perfect absorber and emitter of radiation at this wavelength. If we could see in the deep infrared emitted by the body we would all be nearly black. Under normal conditions, about half our energy loss is through radiation, even if the surrounding environment is not much lower than body temperature.
  • Thermos Flask, invented by James Dewar, Scotland. Coating the inside of an evacuated double walled, glass bottle with a thin layer of silver reduced the heat loss by radiation by a factor of 13. Dewar commissioned a German glass blower to make some, who discovered that milk for his baby stayed warm in the flask overnight. He took the idea of the “Thermos Flasche” to a manufacturer.
  • A glass cake pan will require 20% less baking time than a shiny surfaced pan.

wien’s displacement law

Warm objects are infrared, warmer objects are red hot, even warmer objects are white hot, even more warmer objects are blue hot. Color and temperature are related.

Wien’s displacement law relates the peak wavelength of the thermal radiation emitted by an object to its absolute temperature. First derived by the German physicist Wilhelm Wien in 1893 from a difficult thermodynamic argument that I will not pretend to understand; now derived mathematically from Planck’s law.

λmax = hc 1
k xT

where x is the solution of…

xex  − 5 = 0
ex − 1

x = 4.965114231744276303698759131322893944055584986797250972814…

In shortened form…

λmax = b
T

where…

λmax = (lambda max) the peak wavelength [mm] of the emitted thermal radiation
b = Wien’s displacement constant, 2.898 mmK
T = the absolute surface temperature [K] of the object emitting thermal radiation

A more complete explanation of this law can be found in the section on Planck’s law.

blackbody color by temperature
1,000 K 6,500 K  (daylight) 10,000 K
kelvin
temperature
radiant energy source
2.73 cosmic background radiation
306 human skin
500 household oven at its hottest
660 minimum temperature for incandescence
770 dull red heat
1,400 glowing coals, electric stove, electric toaster
1,900 candle flame
2,000 kerosene lamp
2,800 incandescent light bulb, 75 W
2,900 incandescent light bulb, 100 W
3,000 incandescent light bulb, 200 W
3,100 sunrise or sunset (effective)
3,200 professional studio lights
3,600 one hour after sunrise or one hour before sunset (effective)
4,000 two hours after sunrise or two hours before sunset (effective)
5,500 direct midday sunlight
6,500 daylight (effective)
7,000 overcast sky (effective)
20–30,000 lightning bolt
Temperature (or effective temperature) of selected radiant sources
Color Scale of Temperature

This table is the result of an effort to interpret in terms of thermometric readings, the common expressions used in describing temperatures. It is obvious that these values are only approximations.

Handbook of Chemistry & Physics, Ninth Edition, 1922

color temperature
K
incipient red heat 500–550 770–820
dark red heat 650–750 0920–1020
bright red heat 850–950 1120–1220
yellowish red heat 1050–1150 1320–1420
incipient white heat 1250–1350 1520–1620
white heat 1450–1550 1720–1820
Metal Temperature by Color Source: Process Associates of America
color approximate temperature
K
faint red 930 500 770
blood red 1075 580 855
dark cherry 1175 635 910
medium cherry 1275 0690 0965
cherry 1375 0745 1020
bright cherry 1450 0790 1060
salmon 1550 0845 1115
dark orange 1630 0890 1160
orange 1725 0940 1215
lemon 1830 1000 1270
light yellow 1975 1080 1355
white 2200 1205 1480
T (K) class λmax (nm) color name examples
30,000 O 100 blue NaosMintaka
20,000 B 150 blue-white SpicaRigel
10,000 A 290 white SiriusVega
8000 F 360 yellow-white AdhaferaProcyon
6000 G 480 yellow SunAlpha Centauri
4000 K 720 orange ArcturusAldebaran
3000 M 970 red BetelgeuseRao
Spectral Classification of Stars

solar energy

  • The total global energy consumption of all the humans on the planet is about 1.4 × 1013 W or about one ten-thousandth the total energy from the sun incident on the Earth. The energy use per area in US metropolitan areas is roughly 2% of the incident solar energy.
  • 3.827 × 1026 W total solar luminosity
    1368 W/m2 solar constant (energy perpendicular to direction of propagation)
    0.30 albedo (latin albus, white), surface 0.04, atmosphere 0.26
    342 W/m2 effective solar constant (averaged over time and surface)

greenhouse effect

History

  • Kelvin
  • Arrhenius 1896 estimates CO2 warming
  • Keeling 1960 shows CO2 is increasing
  • Manabe 1967 develop–radiative convective model, first GCM
  • Hansen 1988 GCMs indicate the signal of anthropogenic global climate warming would soon emerge from natural variability
  • Ice cores
  • Mann 1998 Hockey stick graph

The basic effect…

Global temperature and atmospheric carbon dioxide trends match. The very long graph made popular by Al Gore in An Inconvenient Truth.

Plot one against the other. The relation is approximately linear. Al Gore never did this one.

Naturally occurring greenhouse gases whose concentrations are increasing due to human activities

  • CO2 from burning forests and fossil fuels
  • CH4 from rice paddies, cattle, termites (whose population is thought to have increased due to global deforestation), oil fields, and pipeline leaks
  • N2O of agricultural origin

Other naturally occurring greenhouse gases of lesser concern.

  • Water is also a greenhouse gas, but its concentration in the atmosphere is affected by temperature and is not directly affected by human activities.
  • Ozone is also a greenhouse gas but its greenhouse effects are not easily quantified

Greenhouse gases that do not occur naturally.

  • CFCs from from discarded or leaky refrigerators and air conditioners
    Chlorofluorocarbons (CFCs) do not exist naturally, but were invented in the 1930s by researchers at General Motors looking to replace the toxic and corrosive refrigerants in use at the tine: ammonia and sulfur dioxide. CFCs are also implicated in stratospheric ozone loss (the so called “hole” in the ozone layer).
  • HFCs, hydrofluorocarbons
  • HCFCs, hydrocholofluorocarbons
  • PFCs, perfluorocarbons

Indirect greenhouse gases

  • carbon monoxide
  • hydrogen

key infrared absorption bands in the atmosphere correspond to H2O, CO2, O3

Global warming properties of selected greeenhouse gases Source: IPCC and others, * trifluoromethyl sulphur pentafluoride
molecule global warming
potential
(CO2 = 1)
atmospheric
lifetime
(years)
raditative
forcing
(W/m2)
radiative
efficiency
(W/m2ppb)
CO2 carbon dioxide 1 120 1.66 0.000014
CH4 methane 21 12 0.48 0.00037
N2O nitrous oxide 310 114 0.16 0.00303
CCl3F CFC-11 3,800 45 0.063 0.25
CF2Cl2 CFC-12 8,100 100 0.17 0.32
C2F3Cl3 CFC-113 4,800 85 0.024 0.3
CHClF2 HCFC-22 1,500 12 0.033 0.2
CCl4 carbon tetrachloride 1,400 26 0.012 0.13
CH3CCl3 methyl chloroform 146 5 0.0011 0.06
CHF3 HFC-23 11,700 270 0.0033 0.19
C2HF5 HFC-125 2,800 29 0.0009 0.23
C2H2F4 HFC-134a 1,300 14 0.0055 0.16
C2H4F2 HFC-152a 140 1.4 0.0004 0.09
SF6 sulfur hexafluoride 23,900 3,200 0.0029 0.52
SF5CF3 see note below* 19,000 1,000 ? 0.59
H2O water, tropospheric ? ? ? ?
H2O water, stratospheric ? ? 0.02 ?
O3 ozone, tropospheric ? ? +0.35 ?
O3 ozone, stratospheric ? ? −0.15 ?
CO carbon monoxide ? 0.25 ? ?
H2 hydrogen ? ? ? ?

Temperatures are rising across the globe.

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