Imaging Convection and Magnetism in the Sun by Shravan Hanasoge

Author:Shravan Hanasoge
Language: eng
Format: epub
Publisher: Springer International Publishing, Cham

(3.66)

In order to derive kernel expressions for magnetic field, density, and pressure, which are additionally constrained by the equilibrium equation, we consider small perturbations around (3.1), namely

(3.67)

We may ignore perturbations to the gravitational field arising from surface phenomena, such as sunspots or flows in the convection zone, because an overwhelming fraction of solar mass is concentrated within the radiative interior. We have

(3.68)

(3.69)

Terms involving density and magnetic field in the misfit expression for pressure (Eq. [3.70]) are absorbed into kernel expressions for the former two quantities, respectively. The density kernel follows

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