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Herschel/HIFI observations of O-rich AGB stars: molecular inventory

Kay Justtanont (Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium) ; T. Khouri ; Matthias Maercker ; J. Alcolea ; L. Decin ; Hans Olofsson (Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium) ; Fredrik L. Schöier (Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium) ; V. Bujarrabal ; A. P. Marston ; D. Teyssier ; J. Cernicharo ; C. Dominik ; A. de Koter ; G. Melnick ; K. M. Menten ; D. Neufeld ; P. Planesas ; M. Schmidt ; R. Szczerba ; R. Waters
Astronomy and Astrophysics (0004-6361). Vol. 537 (2012), p. Article Number: A144 .
[Artikel, refereegranskad vetenskaplig]

Aims. Spectra, taken with the heterodyne instrument, HIFI, aboard the Herschel Space Observatory, of O-rich asymptotic giant branch (AGB) stars which form part of the guaranteed time key program HIFISTARS are presented. The aim of this program is to study the dynamical structure, mass-loss driving mechanism, and chemistry of the outflows from AGB stars as a function of chemical composition and initial mass. Methods. We used the HIFI instrument to observe nine AGB stars, mainly in the H2O and high rotational CO lines. We investigate the correlation between line luminosity, line ratio and mass-loss rate, line width and excitation energy. Results. A total of nine different molecules, along with some of their isotopologues have been identified, covering a wide range of excitation temperature. Maser emission is detected in both the ortho-and para-H2O molecules. The line luminosities of ground state lines of ortho- and para-H2O, the high-J CO and NH3 lines show a clear correlation with mass-loss rate. The line ratios of H2O and NH3 relative to CO J = 6-5 correlate with the mass-loss rate while ratios of higher CO lines to the 6-5 is independent of it. In most cases, the expansion velocity derived from the observed line width of highly excited transitions formed relatively close to the stellar photosphere is lower than that of lower excitation transitions, formed farther out, pointing to an accelerated outflow. In some objects, the vibrationally excited H2O and SiO which probe the acceleration zone suggests the wind reaches its terminal velocity already in the innermost part of the envelope, i.e., the acceleration is rapid. Interestingly, for R Dor we find indications of a deceleration of the outflow in the region where the material has already escaped from the star.

Nyckelord: stars: AGB and post-AGB, circumstellar matter, stars: late-type, infrared: stars, line: identification, rotational line-profiles, giant branch stars, red supergiant stars, mass-loss history, circumstellar envelopes, water-vapor, w-hydrae, emission, winds, hifi

Denna post skapades 2012-04-12. Senast ändrad 2015-06-23.
CPL Pubid: 156607


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Institutioner (Chalmers)

Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium


Astronomi, astrofysik och kosmologi

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