Global Helioseismology

Abstract

Helioseismology is one of the most successful fields of astrophysics. The observation and characterization of solar oscillation has allowed solar seismologists to study the internal structure and dynamics of the Sun with unprecedented thoroughness. Ground-based networks and dedicated space missions have delivered data of exquisite quality, enabling the development of sophisticated inference techniques. The achievements of the fields count, amongst other, the determination of solar photospheric helium abundance, unacessible to spectroscopic constraints, the precise positioning of the base of the convective zone and the demonstration of the importance of microscopic diffusion in stellar radiative regions. Helioseismology played also a key role in validating the framework used to compute solar and stellar models and played an important role in the so-called solar neutrino problem. In the current era of astrophysics, with the increasing importance of asteroseismology to precisely characterize stars, the Sun still plays a crucial calibration role, acting as a benchmark for stellar models. With the revision of the solar abundances and the current discussions related to radiative opacity computations, the role of the Sun as a laboratory of fundamental physics is undisputable. In this brief review, I will discuss some of the inference techniques developed in the field of helioseismology, dedicated to the exploitation of the solar global oscillation modes.

arXiv commentTo appear in the proceedings of the meeting "How Much do we Trust Stellar Models?" held in Liège in Sept 2018

References in corpus (32)

• The chemical composition of the Sun
• The 'Forbidden' Abundance of Oxygen in the Sun
• Solar Chemical Abundances Determined with a CO5BOLD 3D Model Atmosphere
• Helioseismology and Solar Abundances
• Influence of gravity waves on the internal rotation and Li abundance of solar-type stars
• A new Generation of Standard Solar Models
• Helioseismological Implications of Recent Solar Abundance Determinations
• Line formation in solar granulation VI. [C I], C I, CH and C2 lines and the photospheric C abundance
• A New Generation of Los Alamos Opacity Tables
• Fresh insights on the structure of the solar core
• Asymptotic g modes: Evidence for a rapid rotation of the solar core
• Can Enhanced Diffusion Improve Helioseismic Agreement for Solar Models with Revised Abundances?
• Can plume-induced internal gravity waves regulate the core rotation of subgiant stars?
• Generation of internal gravity waves by penetrative convection
• Large enhancement in high-energy photoionization of Fe XVII and missing continuum plasma opacity
• Constraints on the opacity profile of the sun from helioseismic observables and solar neutrino flux measurements
• Combining multiple structural inversions to constrain the Solar modelling problem
• Fragile detection of solar g modes by Fossat et al
• Line broadening and the solar opacity problem
• Advances in Global and Local Helioseismology: an Introductory Review
• Non linear regularization for helioseismic inversions. Application for the study of the solar tachocline
• Mode Classification in Fast-Rotating Stars using a Convolutional Neural Network: Model-Based Regular Patterns in $\delta$ Scuti Stars
• Determining the metallicity of the solar envelope using seismic inversion techniques
• Comment on "Large enhancement in high-energy photoionization of Fe XVII and missing continuum plasma opacity"
• Helioseismic Measurements in the Solar Envelope Using Group Velocities of Surface Waves
• P-modes in rapidly rotating stars -- looking for regular patterns in synthetic asymptotic spectra
• Solar rotation inversions and the relationship between a-coefficients and mode splittings
• Searching for g modes: Part I. A new calibration of the GOLF instrument
• Inversions of the Ledoux discriminant: a closer look at the tachocline
• Opacity effects on the solar interior. I. Solar structure
• Recalculation of Astrophysical Opacities: Overview, Methodology and Atomic Calculations
• Non-adiabatic pulsations in ESTER models