Jump to content
Main menu
Main menu
move to sidebar
hide
Navigation
Main page
Recent changes
Random page
Help about MediaWiki
Special pages
Niidae Wiki
Search
Search
Appearance
Create account
Log in
Personal tools
Create account
Log in
Pages for logged out editors
learn more
Contributions
Talk
Editing
Spontaneous emission
(section)
Page
Discussion
English
Read
Edit
View history
Tools
Tools
move to sidebar
hide
Actions
Read
Edit
View history
General
What links here
Related changes
Page information
Appearance
move to sidebar
hide
Warning:
You are not logged in. Your IP address will be publicly visible if you make any edits. If you
log in
or
create an account
, your edits will be attributed to your username, along with other benefits.
Anti-spam check. Do
not
fill this in!
==Rate of spontaneous emission== The rate of spontaneous emission (i.e., the radiative rate) can be described by [[Fermi's golden rule]].<ref>B. Henderson and G. Imbusch, Optical Spectroscopy of Inorganic Solids (Clarendon Press, Oxford, UK, 1989).</ref> The rate of emission depends on two factors: an 'atomic part', which describes the internal structure of the light source and a 'field part', which describes the density of electromagnetic modes of the environment. The atomic part describes the strength of a transition between two states in terms of transition moments. In a homogeneous medium, such as [[free space]], the rate of spontaneous emission in the dipole approximation is given by: :<math> \Gamma_{\text{rad}}(\omega)= \frac{\omega^3n|\mu_{12}|^2} {3\pi\varepsilon_{0}\hbar c^3} = \frac{4 \alpha \omega^3n| \langle 1|\mathbf{r}|2\rangle |^2} {3 c^2} </math> :<math> \frac{|\mu_{12}|^2} {\pi\varepsilon_{0}\hbar c} = 4 \alpha | \langle 1|\mathbf{r}|2\rangle |^2 </math> where <math>\omega</math> is the emission frequency, <math>n</math> is the [[index of refraction]], <math>\mu_{12}</math> is the [[transition dipole moment]], <math>\varepsilon_0</math> is the [[vacuum permittivity]], <math>\hbar</math> is the [[reduced Planck constant]], <math>c</math> is the vacuum [[speed of light]], and <math>\alpha</math> is the [[fine-structure constant]]. The expression <math>|\langle 1|\mathbf{r}|2\rangle|</math> stands for the definition of the transition dipole moment <math>|\mu_{12}|=|\langle 1|\mathbf{d}|2\rangle|</math> for dipole moment operator <math>\mathbf{d}=q\mathbf{r}</math>, where <math>q</math> is the elementary charge and <math>\mathbf{r}</math> stands for position operator. (This approximation breaks down in the case of inner shell electrons in high-Z atoms.) The above equation clearly shows that the rate of spontaneous emission in free space increases proportionally to <math>\omega^3</math>. In contrast with atoms, which have a discrete emission spectrum, [[quantum dots]] can be tuned continuously by changing their size. This property has been used to check the <math>\omega^3</math>-frequency dependence of the spontaneous emission rate as described by Fermi's golden rule.<ref>A. F. van Driel, G. Allan, C. Delerue, P. Lodahl, W. L. Vos and D. Vanmaekelbergh, Frequency-dependent spontaneous emission rate from CdSe and CdTe nanocrystals: Influence of dark states, Physical Review Letters, 95, 236804 (2005).[https://journals.aps.org/prl/abstract/10.1103/PhysRevLett.95.236804 Phys. Rev. Lett. 95, 236804 (2005) - Frequency-Dependent Spontaneous Emission Rate from CdSe and CdTe Nanocrystals: Influence of Dark States (aps.org)]</ref>
Summary:
Please note that all contributions to Niidae Wiki may be edited, altered, or removed by other contributors. If you do not want your writing to be edited mercilessly, then do not submit it here.
You are also promising us that you wrote this yourself, or copied it from a public domain or similar free resource (see
Encyclopedia:Copyrights
for details).
Do not submit copyrighted work without permission!
Cancel
Editing help
(opens in new window)
Search
Search
Editing
Spontaneous emission
(section)
Add topic