The abundance of C2H4 in the circumstellar envelope of IRC+10216

TL;DR

This study detects and models ethylene (C2H4) in the circumstellar envelope of IRC+10216, revealing its abundance, distribution, and excitation conditions, with implications for dust chemistry and molecular formation.

Contribution

First high-resolution IR observations of C2H4 in IRC+10216, providing detailed abundance and excitation analysis with a new modeling approach.

Findings

C2H4 abundance is ~6.9E-8 within 5-20R*

C2H4 is mostly formed outward from ~20R*

Up to 25% of C2H4 may condense onto dust grains

Abstract

High spectral resolution mid-IR observations of ethylene (C2H4) towards the AGB star IRC+10216 were obtained using the Texas Echelon Cross Echelle Spectrograph (TEXES) at the NASA Infrared Telescope Facility (IRTF). Eighty ro-vibrational lines from the 10.5 um vibrational mode nu7 with J<30 were detected in absorption. The observed lines are divided into two groups with rotational temperatures of 105 and 400 K (warm and hot lines). The warm lines peak at ~-14 km/s with respect to the systemic velocity, suggesting that they are mostly formed outwards from ~20R*. The hot lines are centered at -10 km/s indicating that they come from a shell between 10 and 20R*. 35% of the observed lines are unblended and can be fitted with a code developed to model the emission of a spherically symmetric circumstellar envelope. The analysis of several scenarios reveal that the C2H4 abundance relative to H2 in the range 5-20R* is 6.9E-8 in average and it could be as high as 1.1E-7. Beyond 20R*, it is 8.2E-8. The total column density is 6.5(3.0)E15 cm^-2. C2H4 is found to be rotationally under local thermodynamical equilibrium (LTE) and vibrationally out of LTE. One of the scenarios that best reproduce the observations suggests that up to 25% of the C2H4 molecules at 20R* could condense onto dust grains. This possible depletion would not influence significantly the gas acceleration although it could play a role in the surface chemistry on the dust grains.