nats 101 updates add your name to class listserve! first quiz on today some textbooks at park &...
Post on 22-Dec-2015
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NATS 101 Updates
• Add your name to Class ListServe!
• First QUIZ on today
• Some textbooks at Park & University Book store
• 1st anniversary of Katrina this week
• Quick update on Ernesto & John
What is Temperature?
Microscopic View
Energy due to random jiggling of molecules
Related to average molecular speed; 500 m/s (=1100 mph) at room temperature for air
Take Home Concepts
• Heat-Energy transfer due to temperature differences
Four modes of heat transfer
Conduction – molecule to molecule
Convection – transport of fluid
Radiation – electromagnetic waves Latent Heat – energy of phase changes
Radiation
• Any object that has a temperature greater than 0 K, emits radiation.
• This radiation is in the form of electromagnetic waves, produced by the acceleration of electric charges.
• These waves don’t need matter in order to propagate; they move at the “speed of light” (3x105 km/sec) in a vacuum.
Electromagnetic Waves
• Two important aspects of waves are:– What kind: Wavelength or distance between
peaks.– How much: Amplitude or distance between peaks
and valleys.
Wavelength
Amplitude Frequency
Why Electromagnetic Waves?
• Radiation has an Electric Field Component and a Magnetic Field Component– Electric Field is Perpendicular to Magnetic Field
Photons
• NOT TO CONFUSE YOU, but…
• Can also think of radiation as individual packets of energy or PHOTONS.
• In simplistic terms, radiation with – shorter wavelengths corresponds to
photons with more energy and – higher wave amplitude to more BB’s per
second
Emitted Spectrum
White Light from Flash Light
Purple GreenRed
•Emitted radiation has many wavelengths.
Prism
(Danielson, Fig. 3.14)
Emitted SpectrumEnergy from Sun is spread unevenly over all wavelengths.
Wavelength
En
erg
y E
mit
ted
Emission spectrum of Sun
Ahrens, Fig. 2.7
Wien’s Law
Relates the wavelength of maximum emission to the temperature of mass
MAX= (0.29104 m K) T-1
Warmer Objects => Shorter Wavelengths• Sun-visible light
MAX= (0.29104 m K)(5800 K)-1 0.5 m• Earth-infrared radiation
MAX= (0.29104 m K)(290 K)-1 10 m
Wien’s Law
What is the radiative temperature of an incandescent bulb whose wavelength of maximum emission is near 1.0 m ?
• Apply Wien’s Law:
MAX= (0.29104 m K) T-1
• Temperature of glowing tungsten filament
T= (0.29104 m K)(MAX)-1
T= (0.29104 m K)(1.0 m)-1 2900K
Stefan-Boltzmann’s (SB) Law
• The hotter the object, the more radiation emitted.
• When the temperature is doubled, the emitted energy increases by a factor of 16!
• Stefan-Boltzmann’s LawE= (5.6710-8 Wm-2K-4 )T4
E=2222=16
4 times
Sun Temp: 6000K
Earth Temp: 300K
Aguado, Fig. 2-7
How Much More Energy is Emitted by the Sun per m2 Than the Earth?• Apply Stefan-Boltzman Law
• The Sun Emits 160,000 Times More Energy per m2 than the Earth,
• Plus Its Area is Mucho Bigger (by a factor of 10,000)!
-2 -2 -4
-2
-2
48
8 4
48
4 544
(W m ) W m K
W mW m
(5.67 10 )
(5.67 10 ) (5800 )5.67 ( )( 10 ) 290
(5800 ) 1.6 1020(290 )
Sun
Earth
E T
E KKE
KK
−
−
−
= ×
×=×
= = ×=
Radiative Equilibrium
• Radiation absorbed by an object increases the energy of the object.– Increased energy causes temperature to
increase (warming).
• Radiation emitted by an object decreases the energy of the object.– Decreased energy causes temperature to
decrease (cooling).
Radiative Equilibrium (cont.)
• When the energy absorbed equals energy emitted, this is called Radiative Equilibrium.
• The corresponding temperature is the Radiative Equilibrium Temperature.
Key Points
• Radiation is emitted from all objects that have temperatures warmer than absolute zero (0 K).
• Wien’s Law: wavelength of maximum emissionMAX= (0.29104 m K) T-1
• Stefan-Boltzmann Law: total energy emissionE= (5.6710-8 W/m2 ) T4
Key Points
• Radiative equilibrium and temperatureEnergy In = Energy Out (Eq. Temp.)
• Three modes of heat transfer due to temperature differences. Conduction: molecule-to-moleculeConvection: fluid motionRadiation: electromagnetic waves