Helioseismology is the study of the structure and dynamics of the Sun through the observation of waves propagating within it. By analyzing these oscillations, which are caused by various types of waves (acoustic, gravity, and surface waves), scientists can gain insights into the Sun's internal structure, including temperature, density, and composition.
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Helioseismology infers the Sun's structure and dynamics from its stellar oscillations. Spatial projection of resolved surface observations onto spherical harmonics identifies angular degree and azimuthal order; a temporal Fourier transform measures mode frequencies. Stellar acoustic modes constrain the adiabatic sound speed, while rotational splitting constrains stellar rotation. Their finite wavelength, surface reflection phases and finite observational coverage limit inversion resolution.