The Nature of Solar Prominences

The evolution of active regions (AR) from their emergence through their long decay process is of fundamental importance in solar physics. Since large-scale flux is generated by the deepseated dynamo, the observed characteristics of flux emergence and that of the subsequent decay provide vital clues as well as boundary conditions for dynamo models. Throughout their evolution, ARs are centres of magnetic activity, with the level and type of activity phenomena being dependent on the evolutionary stage of the AR. As new flux emerges into a pre-existing magnetic environment, its evolution leads to re-configuration of small-and large-scale magnetic connectivities. The decay process of ARs spreads the once-concentrated magnetic flux over an ever-increasing area. Though most of the flux disappears through small-scale cancellation processes, it is the remnant of large-scale AR fields that is able to reverse the polarity of the poles and build up new polar fields. In this Living Review the emphasis is put on what we have learned from observations, which is put in the context of modelling and simulation efforts when interpreting them. For another, modelling-focused Living Review on the sub-surface evolution and emergence of magnetic flux see Fan (2009). In this first version we focus on the evolution of dominantly bipolar ARs. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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“…These late-phase filaments have a greater height and are broader than their predecessors, the "active region filaments" (Tandberg-Hanssen, 1995).…”

Section: Main Laws and Intrinsic Characteristics Of Large-scale Magnementioning

confidence: 98%

Evolution of Active Regions

Driel-Gesztelyi

Green

2015

Living Rev. Sol. Phys.

249

131

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“…The book on the nature of solar prominences by Tandberg-Hanssen (1995) and a recent review of prominence science with emphasis on SOHO contributions by Patsourakos and Vial (2002) cover this subject well and allow us to shorten this section substantially.…”

Section: Prominencesmentioning

confidence: 99%

Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations

et al. 2007

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In Part I of this review, the concepts of solar vacuum-ultraviolet (VUV) observations were outlined together with a discussion of the space instrumentation used for the investigations. A section on spectroradiometry provided some quantitative results on the solar VUV radiation without considering any details of the solar phenomena leading to the radiation. Here, in Part II, we present solar VUV observations over the last decades and their interpretations in terms of the plasma processes and the parameters of the solar atmosphere, with emphasis on the spatial and thermal structures of the chromosphere, transition region and corona of the quiet Sun. In addition, observations of active regions, solar flares and prominences are included as well as of small-scale events. Special sections are devoted to the elemental composition of the solar atmosphere and theoretical considerations on the heating of the corona and the generation of the solar wind.

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“…It was later noted by that the dominant vertical motion in the main body of filaments was oscillatory. Periodic velocities and intensity oscillations have a large range of periodicities, from less than 1 min to hours , Thompson and Schmieder 1991, Balthasar and Wiehr 1994). An excellent review of oscillations in prominence fine-structure is given by Joardar et al (1997), who also discuss and classify hydromagnetic modes of oscillations in thin magnetic strings, which appear to be in good agreement with observations.…”

Section: Flows and Oscillationsmentioning

confidence: 99%

“…The basic properties of solar prominences (filaments) are described and discussed in great details in proceedings and text books (cf., Jensen et al 1979, Poland 1986, Ballester and Priest 1988, Priest 1989, Ruzdjak and TandbergHanssen 1990, and Tandberg-Hanssen 1995. It is the aim of the present review to discuss the physical significance of prominence structure, their dynamics, and relation to the environment.…”

Section: Introductionmentioning

confidence: 98%

Observations of Filament Structure and Dynamics

Engvold¹

1998

International Astronomical Union Colloquium

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Abstract. Past and recent observations of spatial and temporal variations in fine structure of solar prominences/filaments are reviewed. Magnetic fields permeate the prominence plasma and play a decisive role in shaping the fine structure and its dynamics. Consequently, the shape, orientation, and possibly the strength, of the magnetic field may be inferred from the observed sub-structures. The review discusses possible physical implications of small-scale structures in the low-/? prominence plasma.

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The Nature of Solar Prominences

Cited by 469 publications

References 0 publications

Evolution of Active Regions

Evolution of Active Regions

Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations

Observations of Filament Structure and Dynamics

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