Fluorine in a Carbon-enhanced Metal-poor Star

Details Fluorine in a Carbon-enhanced Metal-poor Star Fluorine in a Carbon-enhanced Metal-poor Star

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007apj...667l..81s&link_type=abstract

The Astrophysical Journal, Volume 667, Issue 1, pp. L81-L84.

Astronomy and Astrophysics

Astronomy

21

Stars: Abundances, Stars: Atmospheres, Stars: Carbon, Stars: Individual (He 1305+0132), Stars: Population Ii

Scientific paper

The fluorine abundance of the carbon-enhanced metal-poor (CEMP) star HE 1305+0132 has been derived by analysis of the molecular HF (1-0) R9 line at 2.3357 μm in a high-resolution (R=50,000) spectrum obtained with the Phoenix spectrometer and Gemini-South telescope. Our abundance analysis makes use of a CNO-enhanced ATLAS12 model atmosphere characterized by a metallicity and CNO enhancements determined utilizing medium-resolution (R=3000) optical and near-IR spectra. The effective iron abundance is found to be [Fe/H]=-2.5, making HE 1305+0132 the most Fe-deficient star, by more than an order of magnitude, for which the abundance of fluorine has been measured. Using spectral synthesis, we derive a supersolar fluorine abundance of A(19F)=4.96+/-0.21, corresponding to a relative abundance of [F/Fe]=+2.90. A single line of the Phillips C2 system is identified in our Phoenix spectrum, and along with multiple lines of the first-overtone vibration-rotation CO (3-1) band head, C and O abundances of A(12C)=8.57+/-0.11 and A(16O)=7.04+/-0.14 are derived. We consider the striking fluorine overabundance in the framework of the nucleosynthetic processes thought to be responsible for the C-enhancement of CEMP stars and conclude that the atmosphere of HE 1305+0132 was polluted via mass transfer by a primary companion during its asymptotic giant branch phase. This is the first study of fluorine in a CEMP star, and it demonstrates that this rare nuclide can be a key diagnostic of nucleosynthetic processes in the early Galaxy.

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