The spectrum of the roAp star HD 101065 (Przybylski's star) in the Li I 6708 Å spectral region

Abstract

Abstract. We carried out a detailed analysis of spectra of the unique roAp star HD 101065 (Przybylski's star) near the resonance doublet Li I 6708 Å, using a most complete line list including all possible transitions between REE levels of the NIST database. Our model calculations were performed under two assumptions: a blend of Li and REE lines, and a blend of REE lines only. They prove that Li lines are present in the range 6707.72−6708.02 Å and that the resulting Li abundance is 3.1 dex (in the scale log N(H) = 12.0), while the isotopic ratio 6 Li/ 7 Li is near to 0.3.

High-resolution spectroscopic observations of two chemically peculiar metal-poor stars: HD 10613 and BD+04°2466

“…We were unable to fit this feature with the line of an ion of a heavy element, supposed by Lambert et al (1993) to be a Ce ii line, using the line parameter values (the oscillator strength and the excitation potential) suggested by Lambert et al (1993) and the cerium abundance of BD+04 • 2466 obtained in this work. We included the lines of the rare-earth elements identified around the Li i line by Shavrina et al (2003) in the spectrum of the roAp star HD 101065 (Przybylski's star) highly enriched in the rareearth elements. However, the profile of the absorption feature at 6708 Å cannot be fitted convincingly.…”

On the radioactive shells in peculiar main sequence stars: the phenomenon of Przybylski's star.

“…Shavrina et al (2003) proposed that these reactions can be responsible for the anomalous ratio of lithium isotopes in the atmosphere of PS. Cowley et al (2004) pointed that spallation reactions can produce Tc and Pm in PS.…”

“…These spectra were compared to synthetic spectrum generated using the Kurucz's numeric code SYNTHE and PS atmosphere model calculated by Pavlenko (Shavrina et al 2003) with the following parameters T eff = 6600 K, logg = 4.2 and additional absorption in lines of rare earth elements. The microturbulent velocity of 2.0 km s −1 and projected rotational velocity v sin i = 3.5 km s −1 were adopted.…”

“…Shavrina et al (2003) tried to find new lanthanides lines in the vicinity of Li 6708Å line using NIST energy levels. We are going to make similar investigation for all lines of unstable elements.…”

“…54 elements were investigated by Cowley et al (2000), the abundance of lithium was found by Shavrina et al (2001Shavrina et al ( , 2003, the identification of the lines of Tc and Pm were made by Cowley et al 2 V. F. Gopka et al (2004). This is the second stellar abundance pattern (the first is that of the Sun -73 elements).…”