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Aims: The aim of this work is to verify whether turbulent magneticreconnection can provide the additional energy input required to explain the upto now only poorly understood ionization mechanism of the diffuse ionized gas(DIG) in galaxies and its observed emission line spectra.  Methods: We use a detailed non-LTE radiative transfer code that does not makeuse of the usual restrictive gaseous nebula approximations to compute syntheticspectra for gas at low densities. Excitation of the gas is via an additionalheating term in the energy balance as well as by photoionization. Numericalvalues for this heating term are derived from three-dimensional resistivemagnetohydrodynamic two-fluid plasma--neutral-gas simulations to compute energydissipation rates for the DIG under typical conditions.  Results: Our simulations show that magnetic reconnection can liberate enoughenergy to by itself fully or partially ionize the gas. However, syntheticspectra from purely thermally excited gas are incompatible with the observedspectra; a photoionization source must additionally be present to establish thecorrect (observed) ionization balance in the gas.

astronomy and astrophysics

Numerical Models for the Diffuse Ionized Gas in Galaxies. I. Synthetic  spectra of thermally excited gas with turbulent magnetic reconnection as  energy source