On the possible presence of promethium in the spectra of HD 101065 (Przybylski's star) and HD 965

Details On the possible presence of promethium in the spectra of HD 101065 (Przybylski's star) and HD 965 On the possible presence of promethium in the spectra of HD 101065 (Przybylski's star) and HD 965

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...419.1087c&link_type=abstract

Astronomy and Astrophysics, v.419, p.1087-1093 (2004)

Astronomy and Astrophysics

Astrophysics

17

Stars: Chemically Peculiar, Stars: Abundances, Stars: Activity, Stars: Atmospheres, Methods: Data Analysis

Scientific paper

% Traditional and statistical line-identification methods indicate the presence of Pm I and II, Tc I, and perhaps Tc II in the spectrum of the roAp star HD 101065. These methods also lead to the presence of Pm II and probably also Pm I in a related cool Ap star, HD 965. The spectroscopic evidence is strong enough that we would declare promethium to be present without hesitation, if any of its isotopes were stable. The longest-lived promethium isotope has a half-life of only 17.7 years. The presence of this element would mean that unrecognized processes - perhaps flare activities - are taking place in the atmospheres of these stars. The significance of such processes for galactic chemical evolution cannot be ruled out. We discuss the possibility that the highly improbable wavelength coincidences are due to chance, or due to contamination of the laboratory sources.
Based on observations collected at the European Southern Observatory, La Silla (Chile), as part of programme No. 60.E-0564, and Paranal (Chile), as part of programmes Nos. 68.D-0254 and 70.D-0470.

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