The 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun
Published July 19, 2016 | Version v1
Poster Open

Probing the abundance of SiO and HCN throughout the stellar wind of R Dor

Authors/Creators

  • 1. Instituut voor Sterrenkunde, KU Leuven
  • 2. Chalmers University of Technology, Onsala Space Observatory
  • 3. School of Mathematics and Physics, Queen's University Belfast
  • 4. Leiden Observatory, Leiden University
  • 5. National Astronomical Observatories, Chinese Academy of Sciences

Contributors

  • 1. Uppsala University, University of North Georgia

Description

R Dor is an oxygen-rich AGB star characterised by a low mass-loss rate. Using retrieval methods, we found abundance profiles for SiO and HCN, two chemically important molecules. By comparing these results to those of forward chemistry modelling we will be able to constrain the dominant chemical pathways within the stellar wind. They will also enable us to improve the forward chemistry models, through incorporating dust-gas reactions. The same methodologies will be applied to the abundance profiles retrieved for the O-rich AGB star IK Tau (Decin et al. 2010), which is characterised by a high mass-loss rate.

Files

ProceedingsUppsala.pdf

Files (10.3 MB)

Name Size Download all
md5:045bff35c9f0048e31292d346a1805ae
10.3 MB Preview Download