In physics, the Thermal de Broglie wavelength is defined for a free
ideal gas of massive particles in equilibrium as:
where
The thermal de Broglie wavelength is roughly the average de Broglie wavelength of the gas particles in an ideal gas at the specified temperature. We can take the average interparticle spacing in the gas to be approximately (V/N)1/3 where V is the volume and N is the number of particles. When the thermal de Broglie wavelength is much smaller than the interparticle distance, the gas can be considered to be a classical or Maxwell-Boltzmann gas. On the other hand, when the thermal de Broglie wavelength is on the order of, or larger than the interparticle distance, quantum effects will dominate and the gas must be treated as a Fermi gas or a Bose gas, depending on the nature of the gas particles. The critical temperature is the transition point between these two regimes, and at this critical temperature, the
thermal wavelength will be approximately equal to the interparticle distance.
Massless particles
For a massless particle, the thermal wavelength may be defined as:
where c is the speed of light. As with the massive thermal wavelength, this
is of the order of the average wavelength of the particles in the gas. This is derived from the more general definition of the thermal wavelength due to Yan (Yan 2000)
described below.
General definition of the thermal wavelength
A general definition of the thermal wavelength for an ideal quantum gas in
any number of dimensions and for a generalized relationship between energy and
momentum (dispersion relationship) has been given by Yan (Yan 2000). It is of practical importance, since there are many experimental situations with different dimensionality and dispersion relationships. If n is the number of dimensions, and the relationship
between energy (E) and momentum (p) is given by:
where a and s are constants, then the thermal wavelength is defined as:
![\Lambda=\frac{h}{\sqrt{\pi}}\left(\frac{a}{kT}\right)^{1/s} \left[\frac{\Gamma(n/2+1)}{\Gamma(n/s+1)}\right]^{1/n}](a/../upload/math/ca1050d0e60e7989dcd9094585235a09.png)
where Γ is the Gamma function. For example, in the usual case of massive
particles in a 3-D gas we have n=3 , and E=p2/2m which gives
the above results for massive particles. For massless particles in a 3-D gas,
we have n=3 , and E=pc which gives the above results for massless particles.
References