Physics of Solar Prominences: II—Magnetic Structure and Dynamics

By D. Mackay, J. Karpen, J. Ballester, Brigitte Schmieder, G. Aulanier. 2010

550 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d6672bc3d8ae12b3c9fe28573c8ccccf69004e9b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

COEXISTING FLUX ROPE AND DIPPED ARCADE SECTIONS ALONG ONE SOLAR FILAMENT (2010, unknown): “For reviews of various prominence models, see, e.g., Démoulin (1998) and Mackay et al. (2010).”
Physics of Solar Prominences: I—Spectral Diagnostics and Non-LTE Modelling (2010, background): “2.2.1 and 5 of the companion review paper (Mackay et al. 2010, hereafter Paper II).”
EVOLUTION OF MAGNETIC FIELD AND ENERGY IN A MAJOR ERUPTIVE ACTIVE REGION BASED ON SDO/HMI OBSERVATION (2011, background): “In addition, an interesting “inverse-polarity” configuration (e.g. Mackay et al. 2010, and references therein) exists nearby too, where horizontal field on the photosphere points from negative vertical polarity side to the positive (near “C” in Fig.”
The magnetic field in the solar atmosphere (2014, background): “On larger (active-region) scales, often observed as dark elongated features in Hα 6563 Å and He i 10830 Å images are filaments (“prominences” when observed above the limb; for reviews see Labrosse et al. 2010; Mackay et al. 2010).”
MAGNETIC PROPERTIES OF SOLAR ACTIVE REGIONS THAT GOVERN LARGE SOLAR FLARES AND ERUPTIONS (2016, background): “Thus, this group reminds us of the eruption of a quiescent filament, which is created in the quiet Sun between extended AR remnants, probably with the support of shear flows caused by the differential rotation (Mackay et al. 2010).”