Gravity-mode period spacings and near-core rotation rates of 611 γ Doradus stars with Kepler. Issue 3 (18th October 2019)

• Record Type: Journal Article
• Authors: Li, Gang; Van Reeth, Timothy; Bedding, Timothy R; Murphy, Simon J; Antoci, Victoria; Ouazzani, Rhita-Maria; Barbara, Nicholas H
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 491:Issue 3(2020)
• Page Start: 3586
• Page End: 3605
• Publication Date: 2019-10-18
• Subjects: stars: oscillations -- stars: rotation; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz2906
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We report our survey of γ Dor stars from the 4-yr Kepler mission. These stars pulsate mainly in g modes and r modes, showing period-spacing patterns in the amplitude spectra. The period-spacing patterns are sensitive to the chemical composition gradients and the near-core rotation, hence they are essential for understanding the stellar interior. We identified period-spacing patterns in 611 γ Dor stars. Almost every star pulsates in dipole g modes, while about 30 per cent of stars also show clear patterns for quadrupole g modes and 16 per cent of stars present r-mode patterns. We measure periods, period spacings, and the gradient of the period spacings. These three observables guide the mode identifications and can be used to estimate the near-core rotation rate. We find many stars are hotter and show longer period-spacing patterns than theory. Using the traditional approximation of rotation (TAR), we inferred the asymptotic spacings, the near-core rotation rates, and the radial orders of the g and r modes. Most stars have a near-core rotation rate around 1 d −1 and an asymptotic spacing around 4000 s. We also find that many stars rotate more slowly than predicted by theory for unclear reasons. 11 stars show rotational splittings with fast rotation rates. We compared the observed slope–rotation relation with the theory and find a large spread. We detected rotational modulations in 58 stars and used them to derive the core-to-surface rotation ratios. The interiors rotate faster than the cores in most stars, but by no more than 5 per cent.