Hierarchically modelling Kepler dwarfs and subgiants to improve inference of stellar properties with asteroseismology. Issue 2 (14th May 2021)

• Record Type: Journal Article
• Authors: Lyttle, Alexander J; Davies, Guy R; Li, Tanda; Carboneau, Lindsey M; Leung, Ho-Hin; Westwood, Harry; Chaplin, William J; Hall, Oliver J; Huber, Daniel; Nielsen, Martin B; Basu, Sarbani; García, Rafael A
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 505:Issue 2(2021)
• Page Start: 2427
• Page End: 2446
• Publication Date: 2021-05-14
• Subjects: asteroseismology -- stars: fundamental parameters -- stars: statistics; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab1368
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: With recent advances in modelling stars using high-precision asteroseismology, the systematic effects associated with our assumptions of stellar helium abundance ( Y ) and the mixing-length theory parameter (αMLT ) are becoming more important. We apply a new method to improve the inference of stellar parameters for a sample of Kepler dwarfs and subgiants across a narrow mass range ($0.8 \lt M \lt 1.2\, \rm M_\odot$ ). In this method, we include a statistical treatment of Y and the αMLT . We develop a hierarchical Bayesian model to encode information about the distribution of Y and αMLT in the population, fitting a linear helium enrichment law including an intrinsic spread around this relation and normal distribution in αMLT . We test various levels of pooling parameters, with and without solar data as a calibrator. When including the Sun as a star, we find the gradient for the enrichment law, $\Delta Y / \Delta Z = 1.05\substack{+0.28\\-0.25}$ and the mean αMLT in the population, $\mu _\alpha = 1.90\substack{+0.10\\-0.09}$ . While accounting for the uncertainty in Y and αMLT, we are still able to report statistical uncertainties of 2.5 per cent in mass, 1.2 per cent in radius, and 12 per cent in age. Our method can also be applied to larger samples that will lead to improved constraints on both the population level inference and the star-by-star fundamental parameters.