Radiation| Radiation |
In General > s.a. gauge.
* History: XIX century
pioneers of the study of radiation included Herschel, Melloni and Draper.
@ General references: Dirac PRS(27) [emission and absorption, quantum];
Heald & Marion
95; Kleppner PT(05)feb
[Einstein's 1917 paper]; Milonni PRP(76)
[nr, semiclassical + QED aspects].
@ Observer dependence: Eriksen & Grøn AJP(87)
[Lorentz-invariant]; Nikolic
gq/99 [classical
and quantum]; > s.a. quantum field theory
effects in curved spacetime.
@ Related topics: Schützhold et al PRA(98)qp [non-constant
background, quantum]; Serreau JHEP(04)
[quantum, out of equilibrium]; Chang & Leonelli SHPSA(05)
[ontology, unified vs
pluralistic theory].
Acceleration Radiation, Bremsstrahlung > s.a. electromagnetism;
gravitational radiation;
particle effects.
* Idea: Radiation emitted by an accelerated electric charge.
* Fields: If one solves the wave equation in terms of advanced and
retarded radiation fields, one can separate
AC:= 
(Areta
+ Aadva)
, AR:= (Areta – Aadva)
;
the first one produces the Coulomb field, the second one is responsible for
radiation reaction.
* Larmor equation: The
rate of energy loss for an accelerated non-relativistic charged particle is
dE/dt =
2q2(dv/dt)2/3c3.
* Examples: Synchrotron radiation.
* Issue in curved spacetime:
When a charge is in free fall in a gravitational field, does it radiate or
not? The answer is that a local detector, falling
with it, would not detect radiation, but a distant one not
falling
with it would.
@ General references: in Eyges 72 [Larmor formula]; Holstein & Swift AJP(81)
[elementary derivation]; Ford & O'Connell
PLA(91)
[modification of Larmor equation]; Alexander & Gerlach
PRD(91)gq/99;
Nakel PRP(94);
Matsas PLB(96)gq [Rindler
space]; Chubykalo & Vlaev IJMPA(99)phy/98;
Harpaz & Soker
GRG(98)gq,
FP(01);
Napolitano & Ragusa AJP(99)
[arbitrary motion]; Leinaas ht/98 [e's];
Shariati & Khorrami FPL(99)gq/00 [and
equivalence principle]; Peña et al PRD(05)
[accelerated observers]; Cardoso et al ht/07 [Larmor
formula in higher dimensions]; Huang & Lu FP(08)
[exact expression]; Glass GRG(08) [rev].
@ Uniformly accelerated charge: Fulton & Rohrlich AP(60);
Singal GRG(95),
GRG(97)
[no radiation! – contrary to Parrott GRG(97)gq and
consensus]; Parrott FP(02)gq/93
[and equivalence principle]; Almeida & Saa AJP(06)
[and comoving observers].
@ Synchrotron radiation:
Unruh PRP(98)ht [in electron frame]; Aloisio & Blasi APP(02)ap,
APP(02)ap;
Margaritondo et al RNC(04)
[applications]; Hannay & Jeffrey PRS(05)
[electric field].
@ Extremely relativistic: Gerlach FP(03)gq;
Cardoso et al PRD(03)gq; > s.a.
scattering.
@ In curved spacetime: DeWitt & DeWitt Phys(64);
Matsas GRG(94);
Parrott gq/93 [conformally
flat spacetime], GRG(97)gq;
Higuchi et al PRD(97)gq/96,
Harpaz & Soker GRG(04)phy/99 [static q];
> s.a. quantum field theory effects in curved
spacetime.
@ Accelerating dipole: Power & Thirunamachandran PRS(01),
PRS(01); Gerlach
PRD(01)
[violent acceleration].
@ Accelerated oscillator: Raine et al PRS(91);
Kim & Kim PRD(97);
Kim PRD(99)gq/98 [in
scalar quantum field theory vacuum].
@ And self-force: Hirayama & Hara PTP(00)gq/99; Burko AJP(00)gq/99.
Other Radiation Mechanisms > s.a. casimir
effect [dynamical]; Spontaneous
Emission; Stimulated Emission; thermal
radiation.
* Cerenkov radiation:
Radiation emitted by a particle moving inside a medium at a speed greater than
the speed of light in that medium – the optical
equivalent of a sonic boom; Remark: In a photonic crystal, it is emitted without
a speed threshold, and in the backward direction.
* Inhomogeneous media:
Charged particles radiate when they propagate in inhomogeneous media, even at
constant
velocities; Examples are Ginzburg and Frank's transition radiation, by a particle
crossing
a boundary between different n's, and diffraction radiation near finite-size
objects.
@ Cerenkov: Jelley TPT(63); Balakin et al CQG(01)gq/00 [and
gravitational
waves];
Stevens et al Sci(01)jan [subluminal]; Rohrlich & Aharonov qp/01/PRA
[in
vacuum]; Luo et al Sci(03)jan
+ pw(03)jan
[in
photonic crystal];
Afanasiev 04 [Vavilov-Cherenkov
and synchrotron
radiation]; > s.a. modified electrodynamics, tests
of
lorentz
invariance.
@ Related topics: Diedrich & Walther PRL(87)
[resonance fluorescence of
single ion]; Rabinowitz PT(89)jun-phy/03 [Lilienfeld
transition radiation]; > s.a. branes [diffraction
radiation]; > s.a. gravitating matter.
Interaction and Effects of Radiation > s.a. light.
* Radiation pressure: Related to the energy density u by P = u/3.
* Mössbauer effect:
Recoilless emission/absorption of gamma-rays
by nuclei in solids, in which the whole bulk takes up the momentum so a negligible
amount of energy is given to the solid and the photon energy actually is
the transition energy; Applications:
Used in spectroscopy, can be done when the photon energy is not too high (up
to tens of keV, 57Fe with 14 keV works well)
so that the process can actually be recoilless and not produce phonons; Ether
drift experiments for special relativity, gravitational redshift.
@ General references: Van Vleck & Huber RMP(77)
[with atoms and molecules]; Brivio et al RNC(00);
Gabovich & Gabovich EJP(07)
[mass of radiation in a cavity].
@ Mössbauer effect: Vandegrift & Fultz AJP(98)
[from Schrödinger equation].
@ Radiation pressure: Wu & Ford PRD(01)qp/00 [vacuum fluctuations].
> Propagation effects: see Dichroism; diffraction; dispersion; Reflection; Refraction; wave
phenomena [evanescent].
Radiation Damping, Radiation Reaction and All That > see arrow of time; self-force.
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Send feedback and suggestions to bombelli at olemiss.edu – Modified
11 jul 2008