Atomic Radiative Recombination

Class providing radiative recombination rate coefficients (in cm\(^3\) s\(^{-1}\)) for ions of given atomic number and ionization state at a specified electron temperature. Case A (all recombinations) and case B (excluding recombinations directly to the ground state, for optically thick nebulae) coefficients are supported. These rates are used in ionization equilibrium calculations and in determining the recombination line luminosities of nebulae.

Default implementation: atomicRecombinationRateRadiativeVerner1996

Methods

rate → double precision

Returns the radiative recombination rate in units of cm\(^3\) s\(^{-1}\).

  • integer , intent(in ) :: atomicNumber, ionizationState

  • double precision , intent(in ) :: temperature

  • type (enumerationRecombinationCaseType), intent(in ), optional :: level

atomicRecombinationRateRadiativeComputed

Atomic radiative recombination rates computed from the corresponding photoionization cross section using detailed balance (i.e. the Milne relation—see for example “Astrophysics of the Diffuse Universe” by Dopita & Sutherland, 2004, Springer Science & Business Media, section 5.3.3).

atomicRecombinationRateRadiativeFixed

Computes atomic radiative recombination rates using a fixed, constant rate coefficient specified by [rateCoefficient] in units of cm\(^3\) s\(^{-1}\). This provides a simple, temperature-independent approximation to the recombination rate for use in ionization and cooling calculations.

Parameters

  • [rateCoefficient] (real) — The rate coefficient (in units of cm\(^3\) s\(^{-1}\)) for radiative recombination.

atomicRecombinationRateRadiativeVerner1996

Atomic radiative recombination rates are computed based on the code originally written by Dima Verner.

(Default implementation)