Chemistry of massive young stellar objects with a disk-like structure
| Autor: | Ewine F. van Dishoeck, K. Isokoski, Sandrine Bottinelli |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2013 |
| Předmět: |
Physics
010504 meteorology & atmospheric sciences Young stellar object FOS: Physical sciences Astronomy and Astrophysics Astrophysics Rotation Astrophysics - Astrophysics of Galaxies 01 natural sciences 13. Climate action Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) Phase (matter) 0103 physical sciences Molecule Protostar Outflow 010303 astronomy & astrophysics Excitation 0105 earth and related environmental sciences Line (formation) |
| Zdroj: | Astronomy & Astrophysics, 554, A100 |
| Popis: | Aims: Our goal is to take an inventory of complex molecules in three well-known high-mass protostars for which disks or toroids have been claimed and to study the similarities and differences with a sample of massive young stellar objects (YSOs) without evidence of such flattened disk-like structures. With a disk-like geometry, UV radiation can escape more readily and potentially affect the ice and gas chemistry on hot-core scales. Methods: A partial submillimeter line survey, targeting CH$_{3}$OH, H$_{2}$CO, C$_{2}$H$_{5}$OH, HCOOCH$_{3}$, CH$_{3}$OCH$_{3}$, CH$_{3}$CN, HNCO, NH$_{2}$CHO, C$_{2}$H$_{5}$CN, CH$_{2}$CO, HCOOH, CH$_{3}$CHO, and CH$_{3}$CCH, was made toward three massive YSOs with disk-like structures, IRAS 20126+4104, IRAS 18089-1732, and G31.41+0.31. Rotation temperatures and column densities were determined by the rotation diagram method, as well as by independent spectral modeling. The molecular abundances were compared with previous observations of massive YSOs without evidence of any disk structure, targeting the same molecules with the same settings and using the same analysis method. Results: Consistent with previous studies, different complex organic species have different characteristic rotation temperatures and can be classified either as warm ({gt}100 K) or cold ({lt}100 K). The excitation temperatures and abundance ratios are similar from source to source and no significant difference can be established between the two source types. Acetone, CH$_{3}$COCH$_{3}$, is detected for the first time in G31.41+0.31 and IRAS 18089-1732. Temperatures and abundances derived from the two analysis methods generally agree within factors of a few. Conclusions: The lack of chemical differentiation between massive YSOs with and without observed disks suggest either that the chemical complexity is already fully established in the ices in the cold prestellar phase or that the material experiences similar physical conditions and UV exposure through outflow cavities during the short embedded lifetime. Appendices are available in electronic form at http://www.aanda.org |
| Databáze: | OpenAIRE |
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