Abundance analysis of the supergiant stars HD 80057 and HD 80404 based on their UVES Spectra

TL;DR

This paper analyzes the elemental abundances of two A-type supergiant stars using high-resolution UVES spectra, providing insights into their atmospheric parameters, chemical compositions, and evolutionary status.

Contribution

It presents a detailed abundance analysis of HD 80057 and HD 80404, including new measurements of their atmospheric parameters and chemical compositions, based on high-quality spectral data.

Findings

Abundances of 20-25 elements determined for both stars.

Metallicities close to solar with some elemental deviations.

Stars are in the blue supergiant phase before red supergiant stage.

Abstract

This study presents elemental abundances of the early A-type supergiant HD 80057 and the late A-type supergiant HD80404. High resolution and high signal-to-noise ratio spectra published by the UVES Paranal Observatory Project (Bagnulo et al., 2003) were analysed to compute their elemental abundances using ATLAS9 (Kurucz, 1993, 2005; Sbordone et al., 2004). In our analysis we assumed local thermodynamic equilibrium. The atmospheric parameters of HD 80057 used in this study are from Firnstein & Przybilla (2012), and that of HD80404 are derived from spectral energy distribution, ionization equilibria of Cr I/II and Fe I/II, and the fits to the wings of Balmer lines and Paschen lines as Teff = 7700 +/- 150 K and log g=1.60 +/- 0.15 (in cgs). The microturbulent velocities of HD 80057 and HD 80404 have been determined as 4.3 +/- 0.1 and 2.2 +/- 0.7 km s^-1 . The rotational velocities are 15 +/-1 and 7 +/- 2 km s^-1 and their macroturbulence velocities are 24 +/-2 and 2+/-1 km s^-1 . We have given the abundances of 27 ions of 20 elements for HD 80057 and 39 ions of 25 elements for HD80404. The abundances are close to solar values, except for some elements (Na, Sc, Ti, V, Ba, and Sr). We have found the metallicities [M/H] for HD 80057 and HD 80404 as -0.15 +/- 0.24 and -0.02 +/- 0.20 dex, respectively. The evolutionary status of these stars are discussed and their nitrogen-to-carbon (N/C) and nitrogen-to-oxygen (N/O) ratios show that they are in their blue supergiant phase before the red supergiant region.