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OH/IR stars and their superwinds as observed by the Herschel Space Observatory

Kay Justtanont (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; D. Teyssier ; M. J. Barlow ; M. Matsuura ; B. Swinyard ; Lbfm Waters ; J. Yates
Astronomy and Astrophysics (0004-6361). Vol. 556 (2013),
[Artikel, refereegranskad vetenskaplig]

Aims. In order to study the history of mass loss in extreme OH/IR stars, we observed a number of these objects using CO as a tracer of the density and temperature structure of their circumstellar envelopes. Methods. Combining CO observations from the Herschel Space Observatory with those from the ground, we trace mass loss rates as a function of radius in five extreme OH/IR stars. Using radiative transfer modelling, we modelled the dusty envelope as well as the CO emission. The high-rotational transitions of CO indicate that they originate in a dense superwind region close to the star while the lower transitions tend to come from a more tenuous outer wind which is a result of the mass loss since the early AGB phase. Results. The models of the circumstellar envelopes around these stars suggest that they have entered a superwind phase in the past 200-500 years. The low O-18/O-17 (similar to 0.1 compared to the solar abundance ratio of similar to 5) and C-12/C-13 (3-30 cf. the solar value of 89) ratios derived from our study support the idea that these objects have undergone hot-bottom burning and hence that they are massive M >= 5 M-circle dot AGB stars.

Nyckelord: stars: AGB and post-AGB, stars: mass-loss, submillimeter: stars, asymptotic giant branch, near-infrared photometry, carbon, isotopic-ratios, mass-loss rates, oh-ir sources, evolved stars, agb, stars, circumstellar envelopes, mu-m, quantitative-analysis

Denna post skapades 2013-11-07. Senast ändrad 2015-07-10.
CPL Pubid: 186227


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Institutioner (Chalmers)

Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik (2010-2017)



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