SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 339, 537-544 (1998)

Previous Section Next Section Title Page Table of Contents

5. Discussion

The results of our abundance analyses are given in Table 5, where we also give the results of Conlon et al. (1994) and Dixon & Hurwitz (1998) for Barnard 29 . A comparison of our results with RGB and cooler UV bright stars (only in [FORMULA] Cen) is presented in Figs. 2 and 3. The M 13 data in Fig. 2 are from Smith et al. (1996) and Kraft et al. (1997). The [FORMULA] Cen data for the giants in Fig. 3 were collected from Paltoglou & Norris (1989), Brown et al. (1991), Brown & Wallerstein (1993), and Smith et al. (1995), the data for the cool UVBS are from Gonzalez & Wallerstein (1994). All abundances were adjusted to a solar iron abundance of [FORMULA] = 7.50.

[FIGURE] Fig. 2. The abundances derived for Barnard 29 compared to those of red giant stars in M 13. The solid line connects the abundances derived for Barnard 29 from curve-of-growth analyses. The dotted and short-dashed lines mark the abundances of the red giants taken from Smith et al. (1996) resp. Kraft et al. (1997).

[FIGURE] Fig. 3. The abundances derived for ROA 5701 compared to those of other stars in [FORMULA] Cen. The solid and long-dashed lines connect the abundances derived for ROA 5701 from curve-of-growth and spectrum synthesis analysis, respectively. The short dashed lines mark the cool UV bright stars, the dotted lines connect the abundances of the red giants. For references see text.

As can be seen from Fig. 2 Barnard 29 shows similar abundance trends (except for iron) as the giant stars observed in M 13. This abundance pattern is likely caused by deep mixing and dredge-up of CNO-processed material on the first RGB (Pilachowski et al., 1996). However, the iron abundance we found for Barnard 29 is lower than the cluster value by 0.5 dex. This indicates that the atmosphere of Barnard 29 has become iron depleted during the star's evolution, most likely by the gas-dust separation proposed by Bond (1991) and discussed by Napiwotzki et al. (1994), which is also favoured by Dixon & Hurwitz (1998) for Barnard 29 . This scenario assumes that the dust formed in the cool and extended atmospheres of AGB stars is selectively removed by radiation pressure, while the gas remains at the stellar surface. Since metals with high condensation temperatures (e.g. iron) preferentially condense into dust grains and elements with lower condensation temperatures remain in the gas phase, the remaining gas forms a iron-poor atmosphere. Mathis & Lamers (1992) discussed a single-star and a binary scenario, which can both result in a selective removal of dust at the end of the AGB stage.

The interpretation of the abundance pattern of ROA 5701 is hampered by the complex patterns found in [FORMULA] Cen stars in general (cf. Fig. 3). If we take as a metallicity tracer the sum of C 4, N, and O abundances (which remains unchanged by CNO processing), we find that the original metallicity of ROA 5701 is close to the median value determined for cluster stars (cf. Fig. 4). However, the iron abundance is 0.5 dex below the lowest value found for any RGB star plotted in Fig. 3. This points to an iron depletion similar to that detected in Barnard 29 , which also shows a similar behaviour in Fig. 4.

[FIGURE] Fig. 4. Upper panel: The Fe abundances vs. the sum of CNO abundances for Barnard 29 compared to those of red giants in M 13. For references see text. Lower panel: The Fe abundances vs. the sum of CNO abundances for ROA 5701 compared to those of giants and cool UVBS in [FORMULA] Cen. For references see text.

In summary, the C, N, O, and Si abundances of Barnard 29 and ROA 5701 are in agreement with that of the respective cluster red giant stars. No dredge-up during the AGB phase is necessary to explain these abundance patterns, although a moderate third dredge-up cannot be ruled out from our data alone. However, our low iron abundances point towards a significant iron depletion, most probably caused by a gas-dust separation during the late AGB stages.

Previous Section Next Section Title Page Table of Contents

© European Southern Observatory (ESO) 1998

Online publication: October 21, 1998
helpdesk.link@springer.de