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Table 1

Atmosphere parameters and abundances derived using dynamical models vs. hydrostatic models.

IRAS name Teff (K) log   g β Ṁ(M⊙ yr-1) v (km s-1) [Rb/M]a [Rb/M]staticb [Rb/M]dynb [Zr/M]dynb
Galactic stars
05098−6422 3000 −0.5 1.0 1.0 × 10-8 6 0.1 0.0 ± 0.4 0.0 ± 0.4 ≤0.3 ± 0.3
06300+6058 3000 −0.5 0.2 1.0 × 10-7 12 1.6 1.9 ± 0.4 0.5 ± 0.7 ≤0.1 ± 0.3
18429−1721 3000 −0.5 1.0 1.0 × 10-8 7 1.2 1.2 ± 0.4 1.0 ± 0.4 ≤0.3 ± 0.3
19059−2219 3000 −0.5 0.4 1.0 × 10-7 13 2.3/2.6 2.4 ± 0.4 0.8 ± 0.7 ≤0.3 ± 0.3
LMC star
04498−6842 3400 0.0 1.0 1.0 × 10-7 13 3.9c 3.3 ± 0.4 1.5 ± 0.7 ≤0.3 ± 0.3

Notes.

(a)

See Papers I and II.

(b)

The uncertainties represent the formal errors due to the sensitivity of the derived abundances to slight changes in the model atmosphere parameters (ΔTeff =  ± 100 K, Δ[M/H] = ±0.3, Δξ =  ± 1 km s-1, Δlog  g = +0.5, ΔFWHM = 50 mÅ, Δβ = 0.2, Δlog (/ṀM⊙ yr-1) = 1.0) for each star.

(c)

We scale the Rb overabundance derived by Paper II, [Rb/M] = +5.0, to the adopted LMC metallicity [M/H] = −0.3.

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