| dc.creator |
Pardo Carrión, Juan Ramón |
|
| dc.creator |
Cernicharo, José |
|
| dc.creator |
Goicoechea, Javier R. |
|
| dc.date |
2007-12-28T10:57:50Z |
|
| dc.date |
2007-12-28T10:57:50Z |
|
| dc.date |
2005-07 |
|
| dc.date.accessioned |
2017-01-31T00:59:34Z |
|
| dc.date.available |
2017-01-31T00:59:34Z |
|
| dc.identifier |
The Astrophysical Journal, 628:275–282 (2005) |
|
| dc.identifier |
1538-4357 |
|
| dc.identifier |
http://hdl.handle.net/10261/2629 |
|
| dc.identifier |
10.1086/430774 |
|
| dc.identifier.uri |
http://dspace.mediu.edu.my:8181/xmlui/handle/10261/2629 |
|
| dc.description |
The abundance ratio of consecutive members of the cyanopolyyne family has been explored in CRL 618 using data acquired in a complete line survey covering the frequency range 81–356 GHz. The Jup range explored for the different molecules is 1–4 for HCN and HNC, 9–39 for HC3N, 31–133 for HC5N, and 72–85 for HC7N (not detected beyond Jup=85). The lowest vibrationally excited state of HC7N (nu_15 at 62 cm^-1) has been tentatively detected. Data analysis has been performed by extending our previous geometric and radiative transfermodel of the slowly expanding envelope (SEE) surrounding the compact central continuum source of CRL 618, which was established from the study of rotational lines in several vibrationally excited states of HC3N. The new lines analyzed here require modeling of the high-velocity wind (HVW) component and the colder circumstellar gas, a remnant of the
AGB phase of CRL 618. The derived HC3N/HC5N and HC5N/HC7N abundance ratios from this set of uniformly calibrated lines are between ~3 and 6 in the different regions, similar to standard values in the circumstellar and interstellar media and consistent with previous estimates obtained from ISO observations and chemical models.
However, the abundance ratios of HC3N, HC5N, and HC7N with respect to HCN are at least 2 orders of magnitude larger than those typical for AGB C-rich stars, such as IRC +10216. This fact indicates that in the short transition toward the planetary nebula phase, HCN is quickly reprocessed into longer cyanopolyyne chains. A similar behavior was previously found in this object for the polyacetylenic chains (C2nH2). |
|
| dc.description |
We acknowledge the support of the IRAM 30 m staff during the long completion of the line survey. CSO operations are supported
by US NSF grant AST 22-09008. This work has also been supported by Spanish DGES and PNIE grants ESP 2002-01627, AYA 2002-10113-E, and AYA 2003-02785-E. |
|
| dc.description |
Peer reviewed |
|
| dc.format |
531292 bytes |
|
| dc.format |
application/pdf |
|
| dc.language |
eng |
|
| dc.publisher |
American Astronomical Society |
|
| dc.publisher |
University of Chicago Press |
|
| dc.rights |
openAccess |
|
| dc.subject |
Astrochemistry |
|
| dc.subject |
Circumstellar matter |
|
| dc.subject |
ISM: molecules |
|
| dc.subject |
Radio lines: stars |
|
| dc.subject |
Stars: AGB and post-AGB |
|
| dc.subject |
Stars: carbon |
|
| dc.subject |
Stars: individual (CRL 618) |
|
| dc.title |
Observational evidence of the formation of cyanopolyynes in CRL618 through the polimerization of HCN |
|
| dc.type |
Artículo |
|