Thermal bremsstrahlung

Thermal bremsstrahlung is free-free electromagnetic radiation from the acceleration of charged particles during Coulomb encounters in a thermal plasma. Its frequency-integrated emissivity in a fully ionized, nonrelativistic plasma scales approximately as $n_e{n}_i{T}^{1/2}$.

For a uniform ionized hydrogen column with known temperature and fixed projected angular area, free-free brightness and optical depth depend on $\mathrm{EM}=n_e^{2}L$. The displayed rescaling leaves the whole ideal spectrum unchanged. density and path length cannot be separated without additional information. A known geometry/distance, or a distinct column diagnostic proportional to $n_{e}L$, can break the degeneracy; gas clumping factor and temperature structure complicate that inference.

The fraction $f_V$ of a geometric volume occupied by a specified emitting gas phase is its volume filling factor. For approximately uniform density within that phase, a density-squared luminosity scales as $n_e^2{f}_{V}V$. Without knowledge of $f_V$, emission gives an rms-density combination rather than a unique mean gas density. This filling factor is distinct from the fraction of a telescope beam occupied on the sky.

For a hydrogen-dominated fully ionized plasma, the line-of-sight emission measure is $\mathrm{EM}=\int n_e^{2}dl$. Its units distinguish it from a volume-integrated emission measure $\int n_e^{2}dV$. Thermal free-free optical depth is proportional to $\mathrm{EM}{T}^{-3/2}{\nu }^{-2}{\bar{g}}_{\mathrm{ff}}$ in the radio limit. Inferring density also requires depth, ionization and clumping assumptions.^[ref]

The emission coefficient per volume, frequency and solid angle of a Maxwellian plasma has $j_{\nu }\propto n_e{\sum }_i{Z}_i^2{n}_i{T}^{-1/2}{e}^{-h\nu /(k_{B}T)}{\bar{g}}_{\mathrm{ff}}$. Define the angular convention before supplying a numerical coefficient. The high-frequency cutoff measures temperature, while the normalization measures a density-squared emission integral. The radio spectrum is almost flat when optically thin and rises as ${\nu }^2$ when optically thick at fixed projected area.

For fully ionized hydrogen and helium with hydrogen mass fraction $x_H$, $n_e=(1+x_H)\rho /(2m_p)$ and ${\sum }_i{Z}_i^2{n}_i=\rho /m_p$. With the same unit Gaunt factor for both species, thermal bremsstrahlung at fixed electron number density is multiplied by $2/(1+x_H)$ relative to pure ionized hydrogen. The factor is one for pure hydrogen and two for pure helium.

The Gaunt factor is the dimensionless quantum correction to a classical free-free radiation calculation. Its weak temperature and frequency dependence modifies the approximate thermal bremsstrahlung scaling; a frequency-averaged value appears in the bolometric cooling coefficient.