Improved Laboratory Transition Probabilities for Sm II and Application to the Samarium Abundances of the Sun and Three r-Process-rich, Metal-poor Stars

Details Improved Laboratory Transition Probabilities for Sm II and Application to the Samarium Abundances of the Sun and Three r-Process-rich, Metal-poor Stars Improved Laboratory Transition Probabilities for Sm II and Application to the Samarium Abundances of the Sun and Three r-Process-rich, Metal-poor Stars

Jan 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apjs..162..227l&link_type=abstract

The Astrophysical Journal Supplement Series, Volume 162, Issue 1, pp. 227-260.

Astronomy and Astrophysics

Astronomy

55

Atomic Data, Stars: Abundances, Stars: Population Ii, Sun: Abundances

Scientific paper

Radiative lifetimes, accurate to +/-5%, have been measured for 212 odd-parity levels of Sm II using laser-induced fluorescence. The lifetimes are combined with branching fractions measured using Fourier transform spectrometry to determine transition probabilities for more than 900 lines of Sm II. This work is the largest scale laboratory study to date of Sm II transition probabilities using modern methods. This improved data set has been used to determine a new solar photospheric Sm abundance, logɛ=1.00+/-0.03, from 26 lines. The spectra of three very metal-poor, neutron-capture-rich stars also have been analyzed, employing between 55 and 72 Sm II lines per star. The abundance ratios of Sm relative to other rare earth elements in these stars are in agreement and are consistent with ratios expected from rapid neutron-capture nucleosynthesis (the r-process).

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