Modeling of the Dust and Gas Outflows from OH 26.5+0.6: The Superwind

Details Modeling of the Dust and Gas Outflows from OH 26.5+0.6: The Superwind Modeling of the Dust and Gas Outflows from OH 26.5+0.6: The Superwind

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...456..337j&link_type=abstract

Astrophysical Journal v.456, p.337

Astronomy and Astrophysics

Astronomy

39

Stars: Circumstellar Matter, Ism: Dust, Extinction, Infrared: Stars, Stars: Agb And Post-Agb, Stars: Individual Alphanumeric: Oh 26.5+0.6, Stars: Mass Loss

Scientific paper

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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