Pumping up the [N I] nebular lines

TL;DR

This paper models the [N I] nebular lines, showing FUV pumping explains their strength in some nebulae but not others, and identifies key factors affecting their observed properties.

Contribution

It provides a detailed photoionization model demonstrating the role of FUV pumping in [N I] line emission and clarifies the physical mechanisms influencing line strength and width.

Findings

FUV pumping explains [N I] lines in Orion Nebula but not in planetary nebulae.

The [N I]/Hβ ratio varies with stellar spectral type, matching observations.

Non-thermal broadening of ~5 km/s suggests localized mechanisms like thermal instabilities.

Abstract

The optical [N I] doublet near 5200 {\AA} is anomalously strong in a variety of emission-line objects. We compute a detailed photoionization model and use it to show that pumping by far-ultraviolet (FUV) stellar radiation previously posited as a general explanation applies to the Orion Nebula (M42) and its companion M43; but, it is unlikely to explain planetary nebulae and supernova remnants. Our models establish that the observed nearly constant equivalent width of [N I] with respect to the dust-scattered stellar continuum depends primarily on three factors: the FUV to visual-band flux ratio of the stellar population; the optical properties of the dust; and the line broadening where the pumping occurs. In contrast, the intensity ratio [N I]/H{\beta} depends primarily on the FUV to extreme-ultraviolet ratio, which varies strongly with the spectral type of the exciting star. This is consistent with the observed difference of a factor of five between M42 and M43, which are excited by an O7 and B0.5 star respectively. We derive a non-thermal broadening of order 5 km/s for the [N I] pumping zone and show that the broadening mechanism must be different from the large-scale turbulent motions that have been suggested to explain the line-widths in this H II region. A mechanism is required that operates at scales of a few astronomical units, which may be driven by thermal instabilities of neutral gas in the range 1000 to 3000 K. In an appendix, we describe how collisional and radiative processes are treated in the detailed model N I atom now included in the Cloudy plasma code.