Scattering

In the physical sciences, the wavenumber (also wave number) is the spatial frequency of a wave, either in cycles per unit distance or radians per unit distance. It can be envisaged as the number of waves that exist over a specified distance (analogous to frequency being the number of cycles or radians per unit time).

Because of the use of this term in applied physics, including spectroscopy, often the reference distance should be assumed to be cm. For example, a particle's energy may be given as a wavenumber in cm⁻¹, which strictly speaking is not a unit of energy. However if one assumes this corresponds to electromagnetic radiation, then it can be directly converted to any unit of energy, e.g. 1 cm⁻¹ implies 1.23984×10⁻⁴ eV and 8065.54 cm⁻¹ implies 1 eV.

In multidimensional systems, the wavenumber is also the magnitude of the wave vector.

Definition

It can be defined as either

• $\scriptstyle {\tilde {\nu }}\;=\;{\frac {1}{\lambda }}$, the number of wavelengths per unit distance, where λ is the wavelength, sometimes termed the spectroscopic wavenumber, or
• $\scriptstyle k\;=\;{\frac {2\pi }{\lambda }}$,the number of wavelengths per 2π units of distance, sometimes termed the angular or circular wavenumber, but more often simply wavenumber.

Its usual symbols are $\scriptstyle \nu$, $\scriptstyle {\tilde {\nu }}$, σ or k, the first three used for one definition, the last for another. It has dimensions of reciprocal length, so its SI unit is m⁻¹ and cgs unit cm⁻¹ (in this context formerly called the kayser, after Heinrich Kayser).

For electromagnetic radiation in vacuum, wavenumber is proportional to frequency and to photon energy. Because of this, wavenumbers are used as a unit of energy in spectroscopy. In the SI units, wavenumber is expressed in units of reciprocal meters (m⁻¹), but in spectroscopy it is usual to give wavenumbers in reciprocal centimeters (cm⁻¹). The angular wavenumber is expressed in radians per meter (rad·m⁻¹).

In wave equations

In general, the angular wavenumber $k$ (i.e. the magnitude of the wave vector) is given by

$k={\frac {2\pi }{\lambda }}={\frac {2\pi \nu }{v_{\mathrm {p} }}}={\frac {\omega }{v_{\mathrm {p} }}}$

where $\nu$ is the frequency of the wave, $\lambda$ is the wavelength, $\omega =2\pi \nu$ is the angular frequency of the wave, and v_p is the phase velocity of the wave. The dependence of the wavenumber on the frequency (or more commonly the frequency on the wavenumber) is known as a dispersion relation.

For the special case of an electromagnetic wave in vacuum, where v_p = c, k is given by

$k={\frac {E}{\hbar c}}$

where E is the energy of the wave, ħ is the reduced Planck constant, and c is the speed of light in a vacuum.

For the special case of a matter wave, for example an electron wave, in the non-relativistic approximation:

$k\equiv {\frac {2\pi }{\lambda }}={\frac {p}{\hbar }}={\frac {\sqrt {2mE}}{\hbar }}$

Here p is the momentum of the particle, m is the mass of the particle, E is the kinetic energy of the particle, and ħ is the reduced Planck's constant.

Wavenumber is also used to define the group velocity.

In spectroscopy

In spectroscopy, the wavenumber $\scriptstyle {\tilde {\nu }}$ of electromagnetic radiation is defined as

${\tilde {\nu }}={\frac {1}{\lambda }}$

where λ is the wavelength of the radiation.

The historical reason for using this quantity is that it proved to be convenient in the analysis of atomic spectra. Wavenumbers were first used in the calculations of Johannes Rydberg in the 1880s. The Rydberg–Ritz combination principle of 1908 was also formulated in terms of wavenumbers. A few years later spectral lines could be understood in quantum theory as differences between energy levels, energy being proportional to wavenumber, or frequency. However, spectroscopic data kept being tabulated in terms of wavenumber rather than frequency or energy, since spectroscopic instruments are typically calibrated in terms of wavelength, independent of the value for the speed of light or Planck's constant.

For example, the wavenumbers of the emissions lines of hydrogen atoms are given by

${\tilde {\nu }}=R\left({\frac {1}{{n_{f}}^{2}}}-{\frac {1}{{n_{i}}^{2}}}\right)$

where R is the Rydberg constant and n_i and n_f are the principal quantum numbers of the initial and final levels, respectively (n_i is greater than n_f for emission).

A wavenumber can be converted into energy E via Planck's relation:

$E=hc{\tilde {\nu }}$

It can also be converted into frequency via

${\tilde {\nu }}={\frac {\nu }{c_{\mathrm {n} }}}$

where $\scriptstyle \nu$ is the frequency, and c_n is the speed of light in the medium.

In colloquial usage, the unit cm⁻¹ is sometimes referred to as a "wavenumber", which confuses the name of a quantity with that of a unit. Furthermore, spectroscopists often express a quantity proportional to the wavenumber, such as frequency or energy, in cm⁻¹ and leave the appropriate conversion factor as implied. Consequently, a phrase such as "the energy is 300 wavenumbers" should be interpreted or restated as "the energy corresponds to a wavenumber of 300 cm⁻¹." (Analogous statements hold true for the unit m⁻¹.)

See also

• spatial frequency

References

43 year old Petroleum Engineer Harry from Deep River, usually spends time with hobbies and interests like renting movies, property developers in singapore new condominium and vehicle racing. Constantly enjoys going to destinations like Camino Real de Tierra Adentro.