The solar magnetic field

TL;DR

This paper reviews the Sun's magnetic field, detailing its origin in the solar dynamo, its surface manifestations like sunspots, and its role in heating the corona and driving the solar wind, linking solar interior to heliosphere.

Contribution

It provides a comprehensive overview of the solar magnetic field's structure, origin, and effects, integrating observations and theories across different solar layers.

Findings

Magnetic field generated by the solar dynamo extends from the convection zone to the heliosphere.

Magnetic activity influences solar phenomena such as sunspots, faculae, and solar wind.

Magnetic energy transport heats the solar corona and accelerates the solar wind.

Abstract

The magnetic field of the Sun is the underlying cause of the many diverse phenomena combined under the heading of solar activity. Here we describe the magnetic field as it threads its way from the bottom of the convection zone, where it is built up by the solar dynamo, to the solar surface, where it manifests itself in the form of sunspots and faculae, and beyond into the outer solar atmosphere and, finally, into the heliosphere. On the way it, transports energy from the surface and the subsurface layers into the solar corona, where it heats the gas and accelerates the solar wind.