On the surface physics affecting solar oscillation frequencies

Abstract

Adiabatic oscillation frequencies of stellar models, computed with the standard mixing-length formulation for convection, increasingly deviate with radial order from observations in solar-like stars. Standard solar models overestimate adiabatic frequencies by as much as ~ 20 μHz. In this letter, we address the physical processes of turbulent convection that are predominantly responsible for the frequency differences between standard models and observations, also called `surface effects'. We compare measured solar frequencies from the MDI instrument on the SOHO spacecraft with frequency calculations that include three-dimensional (3D) hydrodynamical simulation results in the equilibrium model, nonadiabatic effects, and a consistent treatment of the turbulent pressure in both the equilibrium and stability computations. With the consistent inclusion of the above physics in our model computation we are able to reproduce the observed solar frequencies to < 3 μHz without the need of any additional ad-hoc functional corrections.

Accepted for publication in Monthly Notices of the Royal Astronomical Society Letters. 5 pages, 5 figures

References in corpus (5)

• Correcting stellar oscillation frequencies for near-surface effects
• ASTEC -- the Aarhus STellar Evolution Code
• A new correction of stellar oscillation frequencies for near-surface effects
• Improvements to stellar structure models, based on a grid of 3D convection simulations. II. Calibrating the mixing-length formulation
• Improvements to Stellar Structure Models, Based on a Grid of 3D Convection Simulations. I. $T(\tau )$-Relations

Cited by in corpus (21)

• Asteroseismology of solar-type stars
• The asteroseismic surface effect from a grid of 3D convection simulations. I. Frequency shifts from convective expansion of stellar atmospheres
• Model-independent measurement of internal stellar structure in 16 Cygni A and B
• Solar $p$-mode damping rates: insight from a 3D hydrodynamical simulation
• Theoretical oscillation frequencies for solar-type dwarfs from stellar models with $⟨3\mathrm{D}⟩$-atmospheres
• 3D Stagger model atmospheres with FreeEOS I. Exploring the impact of microphysics on the Sun
• The amplitude of solar p-mode oscillations from three-dimensional convection simulations
• Mending the structural surface effect of 1D stellar structure models with non-solar metallicities based on interpolated 3D envelopes
• On the computation of eigenfrequencies for equilibrium models including turbulent pressure
• Damping rates and frequency corrections of Kepler LEGACY stars
• The effect of the adiabatic assumption on asteroseismic scaling relations for luminous red giants
• Bayesian inference of stellar parameters based on 1D stellar models coupled with 3D envelopes
• Estimating the nonstructural component of the helioseismic surface term using hydrodynamic simulations
• Surface effects and turbulent pressure. Assessing the Gas-${\Gamma }_1$ and Reduced-${\Gamma }_1$ empirical models
• Testing a non-local 1-equation turbulent convection model: A solar model
• TESS Asteroseismic Analysis of HD 76920: The Giant Star Hosting An Extremely Eccentric Exoplanet
• In search of gravity mode signatures in main sequence solar-type stars observed by Kepler
• Tidally induced stellar oscillations: converting modelled oscillations excited by hot Jupiters into observables
• Spatial incoherence of solar granulation: a global analysis using BiSON 2B data
• Exploring the small-scale magnetic fields of the solar analog KIC 8006161 using asteroseismology
• Can small-scale magnetic fields be the major cause for the near-surface effect of the solar p-mode frequencies?