2014A&A...563A...3P


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.21CET20:52:50

2014A&A...563A...3P - Astronomy and Astrophysics, volume 563A, 3-3 (2014/3-1)

The Be-test in the Li-rich star #1657 of NGC 6397: evidence for Li-flash in RGB stars?

PASQUINI L., KOCH A., SMILJANIC R., BONIFACIO P. and MODIGLIANI A.

Abstract (from CDS):

The Li-rich turn-off star recently discovered in the old, metal-poor globular cluster NGC 6397 could represent the smoking gun for some fundamental, but very rare episode of Li enrichment in globular clusters and in the early Galaxy. We aim to understand the nature of the Li enrichment by performing a spectroscopic analysis of the star, in particular of its beryllium (Be) abundance, and by investigating its binary nature. We used the VLT/UVES spectrograph to observe the near UV region where the BeII resonance doublet and the NH bands are located. We also re-analyzed an archival Magellan/MIKE spectra for C and O abundance determination. We could not detect the BeII lines and derive an upper limit of log(Be/H)←12.2 that is consistent with the Be observed in other stars of the cluster. We could detect a weak G-band, which implies a mild carbon enhancement [C/Fe]+0.4±0.2. We could not detect the UV NH band, showing that this star is less N-enhanced than other stars of the cluster, and we derive an upper limit [N/Fe]<0.0. For oxygen we could not convincingly detect any of the near UV OH lines, which implies that oxygen cannot be strongly enhanced in this star. This is consistent with the detection of the strongest line of the OI triplet at 777nm, which is contaminated by telluric absorptions but is consistent with [O/Fe]∼0.5. Combining the UVES and Mike data, we could not detect any variation in the radial velocity greater than 0.95 km/s over 8 years. The chemical composition of the star strongly resembles that of ``first generation'' NGC 6397 stars, with the huge Li as the only deviating abundance. Not detecting Be rules out two possible explanations of the Li overabundance: capture of a substellar body and spallation caused by a nearby type II SNe. Discrepancies are also found with respect to other accretion scenarios, except for contamination by the ejecta of a star that has undergone the RGB Li-flash. This is at present the most likely possibility for explaining the extraordinary Li enrichment of this star.

Abstract Copyright:

Journal keyword(s): stars: abundances - globular clusters: individual: NGC 6397 - stars: atmospheres

CDS comments: Paragraph 1. 2MASS J17410651-5342290 is a misprint for 2MASS J17410651-5343290.

Simbad objects: 5

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Number of rows : 5

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 V* V822 Cen LXB 14 58 21.9350279092 -31 40 07.515505032 11.95 12.85 12.8     K3-K7V 503 0
2 NGC 6397 GlC 17 40 42.09 -53 40 27.6   7.39 5.17     ~ 1768 1
3 2MASS J17410651-5343290 * 17 41 06.5250255608 -53 43 29.269024594           ~ 3 0
4 NGC 6752 GlC 19 10 52.11 -59 59 04.4   6.96 6.28     ~ 1775 0
5 Cl* NGC 6397 ALA 228 * ~ ~   16.635 16.068     ~ 6 0

    Equat.    Gal    SGal    Ecl

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2020.01.21-20:52:50

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