2014A&A...563L...5D


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.06CET15:24:18

2014A&A...563L...5D - Astronomy and Astrophysics, volume 563, L5-5 (2014/3-1)

The lead discrepancy in intrinsically s-process enriched post-AGB stars in the Magellanic Clouds.

DE SMEDT K., VAN WINCKEL H., KAMATH D., KARAKAS A.I., SIESS L., GORIELY S. and WOOD P.

Abstract (from CDS):

Our understanding of the s-process nucleosynthesis in asymptotic giant branch (AGB) stars is incomplete. AGB models predict, for example, large overabundances of lead (Pb) compared to other s-process elements in metal-poor low-mass AGB stars. This is indeed observed in some extrinsically enhanced metal-poor stars, but not in all. An extensive study of intrinsically s-process enriched objects is essential for improving our knowledge of the AGB third dredge-up and associated s-process nucleosynthesis. We compare the spectral abundance analysis of the SMC post-AGB star J004441.04-732136.4 with state-of-the-art AGB model predictions with a main focus on Pb. The low signal-to-noise (S/N) in the Pb line region made the result of our previous study inconclusive. We acquired additional data covering the region of the strongest Pb line. By carefully complementing re-reduced previous data, with newly acquired UVES optical spectra, we improve the S/N of the spectrum around the strongest Pb line. Therefore, an upper limit for the Pb abundance is estimated from a merged weighted mean spectrum using synthetic spectral modeling. We then compare the abundance results from the combined spectra to predictions of tailored AGB evolutionary models from two independent evolution codes. In addition, we determine upper limits for Pb abundances for three previously studied LMC post-AGB objects. Although theoretical predictions for J004441.04-732136.4 match the s-process distribution up to tungsten (W), the predicted very high Pb abundance is clearly not detected. The three additional LMC post-AGB stars show a similar lack of a very high Pb abundance. From our study, we conclude that none of these low-mass, low-metallicity post-AGB stars of the LMC and SMC are strong Pb producers. This conflicts with current theoretical predictions.

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - stars: evolution - stars: abundances - Magellanic Clouds - stars: chemically peculiar

Simbad objects: 7

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Number of rows : 7

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 OGLE SMC-LPV-4910 pA* 00 44 41.1033737346 -73 21 36.127700113   17.06 15.61 15.44 14.515 G:I 18 0
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9131 1
3 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5398 1
4 2MASS J05063210-7142298 pA? 05 06 32.1298124432 -71 42 29.926032757 14.801 14.717 14.298 13.950 13.780 A3Iab/F0Ibpe 11 0
5 IRAS S05211-6926 LP* 05 20 43.858 -69 23 40.31 17.618 16.515 15.075 13.92 13.887 F5Ib(e) 16 0
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14374 1
7 2MASS J05325071-7139257 LP* 05 32 50.7148448136 -71 39 25.725291413 17.985 16.533 15.069 14.029 13.803 F6Ia 13 0

    Equat.    Gal    SGal    Ecl

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2019.12.06-15:24:18

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