HCN in the inner envelope of {chi} Cygni
| dc.creator | Duari, Debiprosad | |
| dc.creator | Hatchell, Jennifer | |
| dc.date | 2000-06-14 | |
| dc.date.accessioned | 2026-07-07T01:53:57Z | |
| dc.date.available | 2026-07-07T01:53:57Z | |
| dc.description | We have detected the (0,11c,0)J=3-2 and (0,0,0)J=8-7 transitions of HCN towards the S star {chi} Cygni. The excitation requirements of these transitions are too high to be satisfied in the outer envelope of the star, and the emission must originate within {solar}20 stellar radii, ie. the molecule must be forming close to the star. This conclusion is supported by a model for AGB stars in which molecules including HCN form in a shocked wind close to the stellar surface. | |
| dc.description | 4 pages | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0006188 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0006188 | |
| dc.identifier | 2000A&A...358L...25D | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/1163 | |
| dc.subject | Astrophysics | |
| dc.title | HCN in the inner envelope of {chi} Cygni | |
| dc.type | text |