The analysis of promethium abundance in the atmospheres of magnetic-peculiarity stars HD 25354

Heading: 
Physics of Stars and Interstellar Medium
1Yushchenko, VA, 1Gopka, VF, 2Yushchenko, AV, 3Pavlenko, YV, 3Shavrina, AV, 4Musaev, F, 5Demessinova, A
1Scientific Research Institute "Astronomical Observatory" of I.I.Mechnikov Odessa National University, Odesa, Ukraine
2Astrocamp Contents Research Institute, Goyang, Republic of Korea
3Main Astronomical Observatory of the National Academy of Sciences of Ukraine, Kyiv, Ukraine
4Shamakhy Astrophysical Observatory named after N. Tusi of the Azerbaijan National Academy of Sciences, Settlement Y. Mammadaliyev, Shamakhy district, Republic of Azerbaijan, AZ5628
5Faculty of Physics and Technology of the Kazakh National University named after Al Farabi, Alma-Ata, 050040, Kazakhstan
Kinemat. fiz. nebesnyh tel (Online) 2025, 41(1):45-58
https://doi.org/10.15407/kfnt2025.01.045
Language: Ukrainian
Abstract: 

In this paper, we investigate absorption lines of promethium, a radioactive element with a short half-life, in the spectra of magnetic chemically peculiar (MCP) A0Vp star HD 25354 and determine the promethium abundance in the star’s atmosphere. We used an ELODIE archive spectrum of HD 25354 dated 1996 with the wavelength range of 400.0...680.0 nm and the resolving power R = 42,000 obtained with the 1.9-meter telescope at the Haute-Provence Observatory, as well as spectral material with the wavelength range of 370.0...940.0 nm, signal-to-noise ratio up to S/N = 200 for the summed spectrum and the resolving power R = 60,000 obtained by F. Musaev in 2006 with the 2-meter telescope at the Terskol Peak Observatory. Earlier determined atmospheric parameters (Teff = 12,800 K, logg = 4.15 and Vmic = 0.23 km·s–1) and elemental abundances of the star were employed to calculate a synthetic spectrum in the broad range, which, in general, approximated satisfactorily to the observed one, taking into account time variability of profiles and line intensities. When comparing synthetic spectrum of HD 25354 with the observed ones, we identified 11 lines with the predominant contribution of promethium, then determined the promethium content and compared it with the abundances of adjacent lanthanides. The abundance of promethium is found not to extend beyond the range of abundances of other lanthanides, being equal to logN = 5.8...5.9 on the hydrogen scale logN(H) = 12. For comparison, we present the abundances of promethium in the atmosphere of HR 465, which neither exceed logN = 5.05 on the hydrogen scale nor extend beyond the range of lanthanide abundances.
Keywords: abundance, HR465), individual stars (HD25354, magnetic-peculiarity stars, nuclear reactions, nucleosynthesis, promethium

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