Modelling H2 Infrared Emission of the Helix Nebula Cometary Knots
Isabel Aleman, Albert A. Zijlstra, Mikako Matsuura, Ruth Gruenwald,, and Rafael Kimura
TL;DR
This paper uses a photoionisation model to study the infrared emission of molecular hydrogen in the Helix Nebula's cometary knots, explaining observed high excitation temperatures.
Contribution
It introduces a detailed modeling approach to understand H2 emission in nebulae, focusing on the interface regions of cometary knots.
Findings
H2 emission is produced mainly at the H+/H0 interface
The model explains the high excitation temperature of observed H2 lines
Results support the significance of interface regions in nebular emission
Abstract
In the present work, we use a photoionisation code to study the H2 emission of the Helix nebula (NGC 7293) cometary knots, particularly that produced in the interface H+/H0 of the knot, where a significant fraction of the H2 1-0 S(1) emission seems to be produced. Our results show that the production of molecular hydrogen in such region may explain several characteristics of the observed emission, particularly the high excitation temperature of the H2 infrared lines.
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Taxonomy
TopicsAstro and Planetary Science · Stellar, planetary, and galactic studies · Astrophysics and Star Formation Studies