J/A+A/589/A17 Abundance analysis of solar twin HIP 100963 (Yana Galarza+, 2016)
High-precision analysis of the solar twin HIP 100963.
Yana Galarza J., Melendez J., Ramirez I., Yong D., Karakas A.I.,
Asplund M., Liu F.
<Astron. Astrophys. 589, A17 (2016)>
=2016A&A...589A..17Y 2016A&A...589A..17Y (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Stars, fundamental; Sun ; Abundances, [Fe/H]
Keywords: Sun: abundances - stars: abundances - stars: AGB and post-AGB -
stars: fundamental parameters - stars: solar-type - planetary systems
Abstract:
We analyze and investigate the origin of the abundance pattern of HIP
100963 in detail, in particular the pattern of the light element Li,
the volatile and refractory elements, and heavy elements from the s-
and r-processes.
We confirm that HIP 100963 is a solar twin and demonstrate that its
abundance pattern is about solar after corrections for GCE. The star
also shows enrichment in s- and r-process elements, as well as
depletion in lithium that is caused by stellar evolution.
Description:
Stellar abundances [X/H] of HIP 100963 relative to the Sun and
corresponding errors.
Objects:
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RA (2000) DE Designation(s)
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20 28 11.81 +22 07 44.4 HIP 100963 = HD 195034
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 76 26 Stellar abundances of HIP 100963 relative to the Sun
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Element Chemical element
6- 11 F6.3 [-] [X/H] Chemical abundance
15- 19 F5.3 [-] DTeff Errors from effective temperature
23- 27 F5.3 [-] Dlogg Errors from surface gravity
31- 35 F5.3 [-] Dvt Errors from microturbulent velocity
39- 43 F5.3 [-] D[Fe/H] Errors from iron abundance
47- 51 F5.3 [-] param Adding errors in stellar parameters (1)
55- 59 F5.3 [-] obs Observational errors
63- 67 F5.3 [-] Total Total errors
71- 76 F6.3 [-] GCE ? Abundances corrected by subtracting the
chemical evolution of the Galactic
thin disk
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Note (1): For the elements Sc, Ti and Cr, the errors due to uncertainties in the
stellar parameters come from ScII, TiII, CrII, and FeI.
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Acknowledgements:
Jhon Yana Galarza, ramstojh(at)usp.br
(End) Patricia Vannier [CDS] 09-Mar-2016