Structures in the outer solar atmosphere

Abstract

The structure and dynamics of the outer solar atmosphere are reviewed with emphasis on the role played by the magnetic field. Contemporary observations that focus on high resolution imaging over a range of temperatures, as well as UV, EUV and hard X-ray spectroscopy, demonstrate the presence of a vast range of temporal and spatial scales, mass motions, and particle energies present. By focussing on recent developments in the chromosphere, corona and solar wind, it is shown that small scale processes, in particular magnetic reconnection, play a central role in determining the large-scale structure and properties of all regions. This coupling of scales is central to understanding the atmosphere, yet poses formidable challenges for theoretical models.

41 Pages, 15 Figures, Accepted for publication in Space Science Reviews

References in corpus (9)

• Torus instability
• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence
• Highly Efficient Modeling of Dynamic Coronal Loops
• Numerical simulations of fast and slow coronal mass ejections
• Non-equilibrium hydrogen ionization in 2D simulations of the solar atmosphere
• Structure and Dynamics of the Sun's Open Magnetic Field
• Propagation of Alfvénic Waves From Corona to Chromosphere and Consequences for Solar Flares
• Diamagnetic and Expansion Effects on the Observable Properties of the Slow Solar Wind in a Coronal Streamer
• Turbulent Coronal Heating Mechanisms: Coupling of Dynamics and Thermodynamics