Physics of Solar Prominences: II - Magnetic Structure and Dynamics

2010/01/11 by D. H. Mackay, J. T. Karpen, J. L. Ballester +2 · 3 citations
Physics and Astronomy · #astro-ph.SR

paper · pdf · doi:10.1007/s11214-010-9628-0

75 pages, 31 pictures, review paper

arxiv created 2010/01/11 · arxiv updated 2015/05/14

Abstract

Observations and models of solar prominences are reviewed. We focus on non-eruptive prominences, and describe recent progress in four areas of prominence research: (1) magnetic structure deduced from observations and models, (2) the dynamics of prominence plasmas (formation and flows), (3) Magneto-hydrodynamic (MHD) waves in prominences and (4) the formation and large-scale patterns of the filament channels in which prominences are located. Finally, several outstanding issues in prominence research are discussed, along with observations and models required to resolve them.

Cited by

• Can We Distinguish the Source Region Location of Filament/Prominence Eruptions from the Sun-as-a-star Hα Spectrum?
• Initiation Route of Coronal Mass Ejections: II. The Role of Filament Mass
• A New Formation Mechanism of Counterstreaming Mass Flows in Filaments and the Doppler Bullseye Pattern in Prominences

Related

• The Fine Structure of Solar Prominences
• The Formation of Solar Prominences: Plasma Origin and Mechanisms
• The magnetic field of solar prominences
• Simulations of Buoyant Plumes in Solar Prominences
• PROMINENCE FORMATION ASSOCIATED WITH AN EMERGING HELICAL FLUX ROPE