Herschel/HIFI observations of the circumstellar ammonia lines in IRC+10216

TL;DR

This study uses Herschel/HIFI observations and radiative transfer modeling to determine ammonia abundance and distribution in IRC+10216's envelope, highlighting the importance of near-infrared pumping in excitation processes.

Contribution

First detailed analysis of ammonia excitation in IRC+10216 combining high-resolution FIR data with non-LTE modeling including NIR pumping effects.

Findings

NH3 abundance is approximately 3 x 10^{-8} relative to H2.

Ammonia formation occurs near the star, within about 20 stellar radii.

NIR radiative pumping significantly influences NH3 excitation.

Abstract

New high-resolution far-infrared (FIR) observations of both ortho- and para-NH3 transitions toward IRC+10216 were obtained with Herschel, with the goal of determining the ammonia abundance and constraining the distribution of NH3 in the envelope of IRC+10216. We used the Heterodyne Instrument for the Far Infrared (HIFI) on board Herschel to observe all rotational transitions up to the J=3 level (three ortho- and six para-NH3 lines). We conducted non-LTE multilevel radiative transfer modelling, including the effects of near-infrared (NIR) radiative pumping through vibrational transitions. We found that NIR pumping is of key importance for understanding the excitation of rotational levels of NH3. The derived NH3 abundances relative to molecular hydrogen were (2.8+-0.5)x10^{-8} for ortho-NH3 and (3.2^{+0.7}_{-0.6})x10^{-8} for para-NH3, consistent with an ortho/para ratio of 1. These values are in a rough agreement with abundances derived from the inversion transitions, as well as with the total abundance of NH3 inferred from the MIR absorption lines. To explain the observed rotational transitions, ammonia must be formed near to the central star at a radius close to the end of the wind acceleration region, but no larger than about 20 stellar radii (1 sigma confidence level).