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Title:
Modeling of the Dust and Gas Outflows from OH 26.5+0.6: The Superwind
Authors:
Justtanont, K.; Skinner, C. J.; Tielens, A. G. G. M.; Meixner, M.; Baas, F.
Publication:
Astrophysical Journal v.456, p.337 (ApJ Homepage)
Publication Date:
01/1996
Origin:
APJ
ApJ Keywords:
STARS: CIRCUMSTELLAR MATTER, ISM: DUST, EXTINCTION, INFRARED: STARS, STARS: AGB AND POST-AGB, STARS: INDIVIDUAL ALPHANUMERIC: OH 26.5+0.6, STARS: MASS LOSS
DOI:
10.1086/176655
Bibliographic Code:
1996ApJ...456..337J

Abstract

We have observed the extreme OH/IR star, OH 26.5+0.6, in the infrared dust continuum and in the submillimeter rotational lines of CO. Mid-infrared images reveal the compact nature of the circumstellar shell (<0".5). A deep 9.7 microns absorption feature and an absorption at 18 microns show that the dust mass-loss rate is very high. However, the low antenna temperatures of CO J = 1-0 and 2-1 lines suggest that the outer part of the circumstellar shell is much more tenuous. In order to resolve this discrepancy, we have observed the J = 3-2 and 4-3 CO rotational transitions.

We have developed a model for the circumstellar shell for OH 26.5+0.6 which is consistent with the infrared and submillimeter observations. The dust and gas data are well fitted by a two-shell model, consisting of a dense shell surrounded by a more tenuous shell. The former we identify with the superwind (Mdot = 5.5 × 10-4 Msun yr-1), and the latter we identify with mass loss on the asymptotic giant branch (AGB) (Mdot = 10-6Msun yr-1). The transition between the two mass-loss phases is shown to be rather abrupt (Δt < 150 yr). Depending on the mass of the progenitor, this superwind phase may be the last thermal pulse (for M* < 1.5 Msun), or the first of a series of the superwind phases (for up to 8 Msun), punctuated by a period of low mass-loss rates, before the star evolves off the AGB.

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