Stellar Characterization and a Chromospheric Activity Analysis of a K2 Sample of Planet-hosting Stars

• Published in: The Astrophysical journal 2024-07, Vol.970 (1), p.53
• Main Authors: Loaiza-Tacuri, V., Cunha, Katia, Smith, Verne V., Quispe-Huaynasi, F., Costa-Almeida, Ellen, Ghezzi, Luan, Melendez, Jorge
• Format: Article
• Language: English
• Subjects: A stars; Chromospheric activity; Effective temperatures; Exoplanets; Fundamental parameters of stars; Iron; K lines; Local thermodynamic equilibrium; Parallax; Parameter sensitivity; Scattering; Spectroscopy; Stars; Stellar activity; Stellar models; Stellar types
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad4b15

Effective temperatures, surface gravities, and iron abundances were derived for 109 stars observed by the K2 mission using equivalent width measurements of Fe i and Fe ii lines. Calculations were carried out in local thermodynamic equilibrium using Kurucz model atmospheres. Stellar masses and radii were derived by combining the stellar parameters with Gaia Data Release 3 parallaxes, V magnitudes, and isochrones. The derived stellar and planetary radii have a median internal precision of 1.8% and 2.3%, respectively. The radius gap near R planet ∼ 1.9 R ⊕ was detected in this K2 sample. Chromospheric activity was measured from the Ca ii H and K lines using the values of log R HK ′ , which were investigated as a function of stellar rotational period ( P rot ), and we found that chromospheric activity decreases with increasing P rot , although there is a large scatter in log R HK ′ (∼0.5) for a given P rot . The activity levels in this sample reveal a paucity of F and G dwarfs with intermediate activity levels (the Vaughan–Preston gap). The effect that stellar activity might have on the derivation of stellar parameters was investigated by including magnetically sensitive Fe i lines in the analysis and we find no significant differences between parameters with and without magnetically sensitive lines, although the more active stars ( log R HK ′ > − 5.0 ) exhibit a larger scatter in the differences in T eff and [Fe/H].