Asteroseismic masses average 1.29 Msun for Ba dwarfs versus 1.96 Msun for Ba giants, supporting main-sequence accretion evolution from dwarfs to giants, though models fail to match the observed [hs/ls] ratio.
Speagle, A Conceptual Introduction to Markov Chain Monte Carlo Methods arXiv:1909.12313v2, (2020)
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Bayesian inference on observational data yields shear viscosity timescale τ_s=(4.99^{+0.49}_{-0.52})×10^8 T^{5/3} s and bulk viscosity timescale for two-layer hybrid stars, giving frequency minima of 451.87 Hz and 517.47 Hz that explain stability of pulsars including XTE J0929-314.
BBN observations of light nuclei abundances constrain cosmological models with Weylian boundaries via modified Friedmann equations, numerical thermonuclear rate calculations, and MCMC analysis.
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Unveiling the nature of barium stars. I. Asteroseismic masses and the evolutionary link between Ba dwarfs and giants
Asteroseismic masses average 1.29 Msun for Ba dwarfs versus 1.96 Msun for Ba giants, supporting main-sequence accretion evolution from dwarfs to giants, though models fail to match the observed [hs/ls] ratio.
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Modelling Dissipative Dynamics of r-mode Instability in Hybrid Stars
Bayesian inference on observational data yields shear viscosity timescale τ_s=(4.99^{+0.49}_{-0.52})×10^8 T^{5/3} s and bulk viscosity timescale for two-layer hybrid stars, giving frequency minima of 451.87 Hz and 517.47 Hz that explain stability of pulsars including XTE J0929-314.
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Big Bang Nucleosynthesis constraints on the cosmological evolution in a Universe with a Weylian Boundary
BBN observations of light nuclei abundances constrain cosmological models with Weylian boundaries via modified Friedmann equations, numerical thermonuclear rate calculations, and MCMC analysis.