Abstract
The chemistry within the outflow of an AGB star is determined by its elemental C/O abundance ratio. Thanks to the advent of high angular resolution observations, it is clear that most outflows do not have a smooth density distribution, but are inhomogeneous or "clumpy". We have developed a chemical model that takes into account the effect of a clumpy outflow on its gas-phase chemistry by using a theoretical porosity formalism. The clumpiness of the model increases the inner wind abundances of all so-called unexpected species, i.e. species that are not predicted to be present assuming an initial thermodynamic equilibrium chemistry. By applying the model to the distribution of cyanopolyynes and hydrocarbon radicals within the outflow of IRC+10216, we find that the chemistry traces the underlying density distribution.
| Original language | English |
|---|---|
| Pages (from-to) | 531-532 |
| Number of pages | 2 |
| Journal | Proceedings of the International Astronomical Union |
| Early online date | 01 Dec 2019 |
| DOIs | |
| Publication status | Early online date - 01 Dec 2019 |
Keywords
- Astrochemistry
- Circumstellar material
- Molecular processes
- Stars: AGB and post-AGB stars
- Stars: Individual (IRC+10216)
- Stars: Mass loss
ASJC Scopus subject areas
- Medicine (miscellaneous)
- Astronomy and Astrophysics
- Nutrition and Dietetics
- Public Health, Environmental and Occupational Health
- Space and Planetary Science
