15 pages, 5 figures, accepted for publication in The Astrophysical Journal; v2 contains minor changes made in the proofs (updated references & corrected typos)
Recent developments in instrumentation (e.g., in particular the Kepler and CoRoT satellites) provide a new opportunity to improve the models of stellar pulsations. Surface layers, rotation, and magnetic fields imprint erratic frequency shifts, trends, and other non-random behavior in the frequency spectra. As our observational uncertainties become smaller, these are increasingly important and difficult to deal with using standard fitting techniques. To improve the models, new ways to compare their predictions with observations need to be conceived. In this paper we present a completely probabilistic (Bayesian) approach to asteroseismic model fitting. It allows for varying degrees of prior mode identification, corrections for the discrete nature of the grid, and most importantly implements a treatment of systematic errors, such as the "surface effects." It removes the need to apply semi- empirical corrections to the observations prior to fitting them to the models and results in a consistent set of probabilities with which the model physics can be probed and compared. As an example, we show a detailed asteroseismic analysis of the Sun. We find a most probable solar age, including a 35 +- 5 million year pre-main sequence phase, of 4.591 billion years, and initial element mass fractions of X_0 = 0.72, Y_0 = 0.264, Z_0 = 0.016, consistent with recent asteroseismic and non-asteroseismic studies.
Improvements to Asteroseismic Fitting of White Dwarfs in the Gaia Era
City University of New York Graduate Center（纽约市立大学研究生中心）；Queens College（皇后学院）；American Museum of Natural History（美国自然历史博物馆）；Penn State Wilkes-Barre（宾夕法尼亚州立大学威尔克斯-巴里分校）
Asteroseismic modelling of main-sequence solar-like stars and Kepler exoplanet host stars with the FICO procedure I. Catalogue of fundamental stellar properties
Uppsala University（乌普萨拉大学）；Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS（巴黎天文台，巴黎文理研究大学，索邦大学，巴黎西岱大学，CY塞吉-蓬图瓦兹大学，法国国家科学研究中心）；STAR Institute, Université de Liège（列日大学天体物理、恒星和系外行星研究所）；Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP（波尔图大学空间科学与天体物理研究所）
Glitch analysis and asteroseismic modelling of subgiant $μ$ Herculis: confirming and interpreting the $Γ_1$ peak as the helium glitch
Department of Physics, Indian Institute of Technology (BHU), Varanasi 221005, India（印度瓦拉纳西印度理工学院（贝拿勒斯 Hindu 大学）物理系）；Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus, Denmark（丹麦奥胡斯大学天体物理学中心（SAC），物理与天文系）；School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK（英国伯明翰大学物理与天文学院）；DARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, 18, 2200, Copenhagen, Denmark（丹麦哥本哈根大学尼尔斯·玻尔研究所 DARK 中心）；Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain（西班牙特内里费岛拉古纳加那利群岛天体物理研究所）；Universidad de La Laguna (ULL), Departamento de Astrofísica, 38206 La Laguna, Tenerife, Spain（西班牙特内里费岛拉古纳拉古纳大学天体物理系）
Flow-Based Generative Emulation of Grids of Stellar Evolutionary Models
Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所）；Institute for Astronomy, University of Hawai‘i（夏威夷大学天文研究所）
Surface brightness-color relations for red giant branch stars: Observational constraints on metallicity effects using the ARD method
Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Key Laboratory for Structure and Evolution of Celestial Objects, Chinese Academy of Sciences（中国科学院天体结构与演化重点实验室）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of the Chinese Academy of Sciences（中国科学院大学）
