The solar magnetic field

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.

83 pages, 42 figures, about 2.5 MB in size

References in corpus (8)

• Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope
• A Substantial Amount of Hidden Magnetic Energy in the Quiet Sun
• The case for a distributed solar dynamo shaped by near-surface shear
• On magnetic field generation in Kolmogorov turbulence
• Comparing magnetic field extrapolations with measurements of magnetic loops
• Similarities and Differences between Coronal Holes and the Quiet Sun: Are Loop Statistics the Key?
• Strong mean field dynamos require supercritical helicity fluxes
• Magnetic modelling and tomography: First steps towards a consistent reconstruction of the solar corona

Cited by in corpus (12)

• The Solar Optical Telescope for the Hinode Mission: An Overview
• On the role of meridional flows in flux transport dynamo models
• Chromospheric magnetic field and density structure measurements using hard X-rays in a flaring coronal loop
• Stokes diagnostics of simulated solar magneto-convection
• Interpretation of Solar Magnetic Field Strength Observations
• The Magnetic Sun: Reversals and Long-Term Variations
• Discriminant analysis of solar bright points and faculae I. Classification method and center-to-limb distribution
• On the possibility of a bimodal solar dynamo
• SUMER observations of the inverse Evershed effect in the transition region above a sunspot
• 3D Numerical Simulations of f-Mode Propagation Through Magnetic Flux Tubes
• An analytic interface dynamo over a shear layer of finite depth
• Magnetic field contribution to the last electron-photon scattering