Pulsational properties of ten new slowly pulsating B stars

TL;DR

This study analyzes ten newly identified SPB stars using photometric data and stellar models to determine their pulsational modes, stellar parameters, and evolutionary status, demonstrating ground-based observations' effectiveness in asteroseismology.

Contribution

The paper presents the first detailed pulsational analysis of ten new SPB stars, expanding the sample with mode identifications and stellar parameters for improved stellar modeling.

Findings

Identified pulsational frequencies and modes for ten SPB stars.

Constrained stellar parameters such as mass and age for several stars.

Demonstrated ground-based photometry's viability for asteroseismology.

Abstract

We collected a sample of ten hitherto unidentified SPB stars with the aim of describing their pulsational properties and identifying pulsational modes. Photometric time series data from various surveys were collected and analyzed using diverse frequency search algorithms. We calculated astrophysical parameters and investigated the location of our sample stars in the \logTeff\ versus \logl\ diagram. Current pulsational models were calculated and used for the identification of pulsational modes in our sample stars. An extensive grid of stellar models along with their g-mode eigenfrequencies was calculated and subsequently cross-matched with the observed pulsational frequencies. The best-fit models were then used in an attempt to constrain stellar parameters such as mass, age, metallicity, and convective overshoot. We present detected frequencies, corresponding g-mode identifications, and the masses and ages of the stellar models producing the best frequency cross-matches. We partially succeeded in constraining stellar parameters, in particular concerning mass and age. Where applicable, rotation periods have been derived from the spacing of triplet component frequencies. No evolved SPB stars are present in our sample. We identify two candidate high-metallicity objects (HD\,86424 and HD\,163285), one young SPB star (HD\,36999), and two candidate young SPB stars (HD\,61712 and HD\,61076). We demonstrate the feasibility of using ground-based observations to perform basic asteroseismological analyses of SPB stars. Our results significantly enlarge the sample of known SPB stars with reliable pulsational mode identifications, which provides important input parameters for modeling attempts aiming to investigate the internal processes at work in upper main-sequence stars.