Thermal
or Black-Body Radiation| Thermal
or Black-Body Radiation |
In General > s.a. radiation.
* Idea: Radiation emitted
by a perfectly absorbing and emitting body at a fixed temperature T;
The calculation of its spectrum was "a loose thread that
when tugged (by Planck) would eventually unravel the entire fabric of what
had passed for reality."
* Spectrum: It is given by the Planck distribution
E(f, T) df = (2
h/c2)
(f 3 / ehf/kT –1)
df .
* Stefan-Boltzmann law: For
a black body at temperature T,
the total energy emitted per unit surface and unit time is E = 
T 4,
with
the Stefan-Boltzmann
constant.
* Wien's law: For a black body at temperature T, 
max
= (0.0029 m/K) T –1.
References
@ General: Planck 06; Agnese et al NCB(99)
[simple]; Chang & Guan qp/04 [in
a compact space]; Boyer FP(07)
[and relativity and discrete charge]; Kramm & Herbert a0801 [using
dimensional analysis].
@ Quantum aspects:
Boya et al qp/00 [multiphoton
states]; Greffet et al Nat(02)mar,
Greffet & Henkel CP(07)
[coherent emission]; Johansen JOB(04)qp.
@ History: Boya RACZ(03)phy/04 [Planck
1900]; Varró FNL(06)qp [Einstein's
fluctuation formula].
@ Coupling to atoms: Fröhlich & Merkli
CMP(04)mp [return to equilibrium].
@ Classical derivation: Marshall NC(65); Boyer
PRD(84) [from equivalence principle and zero-point
radiation].
@ Related topics: Silva e Costa PLA(04)
[as seen by moving observer].
@ Variations: Kim et al a0705-PRD
[in 
-Minkowski
spacetime]; García-García a0709 [finite-size
corrections].
Main page – Abbreviations – Journals – Comments – Other
sites – Acknowledgements
Send feedback and suggestions to bombelli at olemiss.edu – Modified
16 jan 2008