Effects of X-ray irradiation and disk flaring on the [NeII] 12.8 micron emission from young stellar objects

TL;DR

This study investigates how X-ray irradiation and disk structure influence the [Ne II] 12.8 micron emission in young stellar objects, explaining observed luminosity scatter and providing insights into disk geometry.

Contribution

It demonstrates that star-disk parameters like X-ray hardness and disk flaring significantly affect [Ne II] emission, offering explanations for observational variability.

Findings

Variations in star-disk parameters can cause up to an order of magnitude change in [Ne II] luminosity.

Disk flaring impacts the size of the emission region and line profile.

Hardness of X-ray spectrum has limited effect on line profiles.

Abstract

The [Ne II] fine-structure emission line at 12.8 micron has been detected in several young stellar objects (YSO) spectra. This line is thought to be produced by X-ray irradiation of the warm protoplanetary disk atmospheres, however the observational correlation between [Ne II] luminosities and measured X-ray luminosities shows a large scatter. Such spread limits the utility of this line as a probe of the gaseous phase of disks, as several authors have suggested pollution by outflows as a probable cause of the observed scatter. In this work we explore the possibility that the large variations in the observed [Ne II] luminosity may be caused instead by different star-disk parameters. In particular we study the effects that the hardness of the irradiating source and the structure (flaring) of the disk have on the luminosity and spectral profile of the [Ne II] 12.8 micron line. We find that varying these parameter can indeed cause up to an order of magnitude variation in the emission luminosities which may explain the scatter observed, although our models predict somewhat smaller luminosities than those recently reported by other authors who observed the line with the Spitzer Space Telescope. Our models also show that the hardness of the spectrum has only a limited (undetectable) effect on the line profiles, while changes in the flaring power of the disk significantly affect the size of the [Ne II] emission region and, as a consequence, its line profile. In particular we suggest that broad line profiles centred on the stellar radial velocity may be indicative of flat disks seen at large inclination angles.