Save Money and Energy by Detecting Heat Losses
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This document discusses quantitative thermography and infrared radiation. It explains that infrared is emitted, reflected, transmitted, and absorbed, with the amount depending on temperature. It presents the equations of Planck's law and Stefan-Boltzman's law that describe blackbody radiation as a function of temperature and wavelength. Convection heat transfer is also discussed. The document provides examples of calculating heat loss from pipes and annual savings from insulating pipes to reduce heat loss. It concludes with questions about calculating potential annual savings from insulating pipes.
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1) Classical theories could not explain the spectrum of blackbody radiation, predicting infinite energy at short wavelengths.
2) Planck hypothesized that the oscillators could only emit or absorb energy in discrete quantized units proportional to frequency, avoiding the infinity.
3) This led to Planck's law of radiation, which correctly described the blackbody spectrum using a quantum of action hν. This founding of quantum theory resolved the ultraviolet catastrophe.
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2) Planck hypothesized that the oscillators could only emit or absorb energy in discrete quantized units proportional to frequency, avoiding the infinity.
3) This led to Planck's law of radiation, which correctly described the blackbody spectrum using a quantum of action hν. This founding of quantum theory resolved the ultraviolet catastrophe.
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- The Rayleigh-Jeans law, derived from classical physics, correctly predicted blackbody radiation at long wavelengths but failed at short wavelengths, known as the ultraviolet catastrophe. Planck's hypothesis resolved this issue.
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- Kirchhoff's law states that for a body in thermal equilibrium, the emissive power and absorptive power are equal for each wavelength.
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The document discusses several key concepts relating to blackbody radiation:
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2) Stefan-Boltzmann law describes the amount of radiant energy emitted from a black body, which absorbs all radiation.
3) Planck's law defines the emissive power of a black body as a function of wavelength and temperature.
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2. Using strings with different linear mass densities allows a piano manufacturer to use strings with lengths that are all the same order of magnitude by accommodating extremely high frequencies on relatively short strings.
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2) In 1924, Louis de Broglie postulated that all matter has an intrinsic wavelength that is related to its momentum, not just light. He derived that the wavelength λ of a particle with momentum p is given by λ = h/p, where h is Planck's constant.
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2) 13C NMR spectra contain information about the number and types of carbon atoms present based on the number of signals and their chemical shifts. The chemical shifts are influenced by factors like hybridization and electronegativity.
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surfaces has attracted considerable interest due to its
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CCSD(T)-based relaxed potential energy curves for the
attack of atomic hydrogen on a center carbon atom of
pyrene and coronene at a tiny fraction of the computational
cost. Using this cheap quantum chemical potential, we performed direct on-the-fly Born-Oppenheimer
MD simulations while “shooting” H atoms with varying collision energies on a periodic graphene target
equilibrated at 300 Kelvin. We compared reaction cross sections for a) elastic collisions, b)
chemisorption reactions, c) penetration reactions in dependence of H/D/T kinetic energies, and found
remarkable differences to previously reported classical MD simulations of the same process. Using the
same potential, in simulations involving the shooting of up to 400 hydrogen atoms on the graphene sheet,
we observed the self-assembly of C4H, a novel polymer with localized aromatic hexagons, in agreement
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The document discusses several key concepts relating to blackbody radiation:
1) A blackbody is an idealized object that absorbs all electromagnetic radiation falling on it without reflecting or transmitting any.
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KPI nel carrello: 27 indicatori di successo di un eCommerce
KPI nel carrello: 27 indicatori di successo di un eCommerce
конспект урока что мы узнали о полезных ископаемых.
конспект урока что мы узнали о полезных ископаемых.
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Save Money and Energy by Detecting Heat Losses
- 1. Quantitative Thermography Temperature and Tantrums
- 2. Infrared – What is it?
- 3. How is it emitted? E = hv Frequency of radiation, sometimes written as f giving expression E=hf. Quantum energy of a photon. H – Planck’s constant = 6.626 x 10 Joule-sec = 4.136 x 10 eV-s -34 -15
- 4. The Weird World of Infrared What is this?
- 5. Emitted (Tg) Reflected (Tr) Transmitted (Tt) The Weird World of Infrared – Part 2 AbsorbedBackground (Tb) Gas “Cloud”
- 6. Radiation Laws Planck’s Law The formula describing the spectral radiation of a perfect blackbody as a function of its temperature and the wavelength of the emitted radiation Wλb = 2π h c2 x 10-6 [ W/m2(µm)] λ5 (ehc/λkT – 1) h-=Planck’s constant k=Boltzman’s contstant Stefan-Boltzmann’s Law The formula indicates the total radiation at ALL wavelengths from a perfect blackbody W[TOTAL] = 5.67 x 10-8 T4 [W/m2]
- 7. Convection For horizontal pipes WConvection = 1.35 x (Ts – Ta)0.25 / dop [ W/m2] Ts = Absolute temperature of heat emitting surface Ta = Absolute temperature of air dop = Outside diameter of pipe/insulation
- 9. Total loss in horizontal pipework Q = length π dop (WConvection + WRadiation) = length x π dop x (1.35 x (Ts – Ta)0.25 / dop + 5.67 x 10-8 T4)
- 10. Examples
- 11. Examples
- 12. Examples
- 13. Quiz – How much per year? £10,811 £33,000pa for 25mph wind
- 14. Quiz – How much £21,500 £73,000pa for 25mph wind
- 15. Thank you for Listening Any Questions?