Transition probabilities of astrophysical interest in the niobium ions Nb and Nb

¹ Lund Observatory, Lund University, Box 43, 221 00 Lund, Sweden e-mail: hampus.nilsson@astro.lu.se
² Department of Physics, Lund University, Box 118, 221 00 Lund, Sweden
³ Department of Astronomy, University of Texas, RLM 15.308, Austin TX78712, USA
⁴ Astrophysique et Spectroscopie, Université de Mons, 20 Place du Parc, 7000 Mons, Belgium
⁵ IPNAS, Bât. B15, Université de Liège, Sart Tilman, 4000 Liège, Belgium

Received: 29 October 2009
Accepted: 20 November 2009

Abstract

Aims. We attempt to derive accurate transition probabilities for astrophysically interesting spectral lines of and and determine the niobium abundance in the Sun and metal-poor stars rich in neutron-capture elements.

Methods. We used the time-resolved laser-induced fluorescence technique to measure radiative lifetimes in . Branching fractions were measured from spectra recorded using Fourier transform spectroscopy. The radiative lifetimes and the branching fractions were combined yielding transition probabilities. In addition, we calculated lifetimes and transition probablities in and using a relativistic Hartree-Fock method that includes core polarization. Abundances of the sun and five metal-poor stars were derived using synthetic spectra calculated with the MOOG code, including hyperfine broadening of the lines.

Results. We present laboratory measurements of 17 radiative lifetimes in . By combining these lifetimes with branching fractions for lines depopulating the levels, we derive the transition probabilities of 107  lines from 4d³5p configuration in the wavelength region 2240-4700 Å. For the first time, we present theoretical transition probabilities of 76 Nb III transitions with wavelengths in the range 1430-3140 Å. The derived solar photospheric niobium abundance log  = 1.44 ± 0.06 is in agreement with the meteoritic value. The stellar Nb/Eu abundance ratio determined for five metal-poor stars confirms that the r-process is a dominant production method for the n-capture elements in these stars.