Plasma Structure and Dynamics

Karpen, J. T.

doi:10.1007/978-3-319-10416-4_10

Cited by 16 publications

(16 citation statements)

References 130 publications

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“…However, magnetic field geometry (e.g., dipped or flat field lines) is expected to play an important role in establishing where prominences form (see Karpen, 2014 and references therein).…”

Section: Continuum Absorptionmentioning

confidence: 99%

FORWARD: A Toolset for Multiwavelength Coronal Magnetometry

Gibson

Kucera

White

et al. 2016

Front. Astron. Space Sci.

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Determining the 3D coronal magnetic field is a critical, but extremely difficult problem to solve. Since different types of multiwavelength coronal data probe different aspects of the coronal magnetic field, ideally these data should be used together to validate and constrain specifications of that field. Such a task requires the ability to create observable quantities at a range of wavelengths from a distribution of magnetic field and associated plasma-i.e., to perform forward calculations. In this paper we describe the capabilities of the FORWARD SolarSoft IDL package, a uniquely comprehensive toolset for coronal magnetometry. FORWARD is a community resource that may be used both to synthesize a broad range of coronal observables, and to access and compare synthetic observables to existing data. It enables forward fitting of specific observations, and helps to build intuition into how the physical properties of coronal magnetic structures translate to observable properties. FORWARD can also be used to generate synthetic test beds from MHD simulations in order to facilitate the development of coronal magnetometric inversion methods, and to prepare for the analysis of future large solar telescope data.

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“…However, magnetic field geometry (e.g., dipped or flat field lines) is expected to play an important role in establishing where prominences form (see Karpen, 2014 and references therein).…”

Section: Continuum Absorptionmentioning

confidence: 99%

FORWARD: A Toolset for Multiwavelength Coronal Magnetometry

Gibson

Kucera

White

et al. 2016

Front. Astron. Space Sci.

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“…In particular, the abiding presence of a prominence implies a magnetic structure that can provide sustained gravitational support and thermal isolation. Several excellent review chapters within the recent book Solar Prominences (Engvold and Vial 2015) cover our theoretical understanding of the origins of such magnetic structures and their evolution on a variety of temporal and spatial scales (Mackay 2015), the energetic processes associated with prominence formation and visibility (Gilbert 2015; Heinzel 2015; Karpen 2015), and the mechanisms responsible for the ultimate fate of many prominences as the cores of solar eruptions (Fan 2015). Prominence observations and interpretation are also well-covered by other chapters within that book (Ballester 2015; Engvold 2015; Gibson 2015; Gopalswamy 2015; Kucera 2015; Labrosse 2015; López Ariste 2015; Lugaz 2015; Martin 2015; Parenti 2015; Webb 2015) and by the Living Reviews on “Prominence Oscillations” by Arregui et al.…”

Section: Introductionmentioning

confidence: 99%

Solar prominences: theory and models

Gibson

2018

Living Rev Sol Phys

108

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Magnetic fields suspend the relatively cool material of solar prominences in an otherwise hot corona. A comprehensive understanding of solar prominences ultimately requires complex and dynamic models, constrained and validated by observations spanning the solar atmosphere. We obtain the core of this understanding from observations that give us information about the structure of the “magnetic skeleton” that supports and surrounds the prominence. Energetically-sophisticated magnetohydrodynamic simulations then add flesh and blood to the skeleton, demonstrating how a thermally varying plasma may pulse through to form the prominence, and how the plasma and magnetic fields dynamically interact.

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“…As yet this mass loading procedure has not been identified. One of the possible mechanisms of prominence formation-the thermal nonequilibrium evaporation-condensation model-was developed by Antiochos et al (1999) and has been further explored by e.g., Karpen et al (2006), Luna et al (2012), Xia & Keppens (2016), see also Karpen (2015). This mechanism produces a deposition of the prominence plasma onto individual field lines or smallscale bundles of them.…”

Section: Discussionmentioning

confidence: 99%

Properties of the prominence magnetic field and plasma distributions as obtained from 3D whole-prominence fine structure modeling

Gunár

Mackay

2016

A&A

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Aims. We analyze distributions of the magnetic field strength and prominence plasma (temperature, pressure, plasma β, and mass) using the 3D whole-prominence fine structure model. Methods. The model combines a 3D magnetic field configuration of an entire prominence, obtained from non-linear force-free field simulations, with a detailed semi-empirically derived description of the prominence plasma. The plasma is located in magnetic dips in hydrostatic equilibrium and is distributed along multiple fine structures within the 3D magnetic model. Results. We show that in the modeled prominence, the variations of the magnetic field strength and its orientation are insignificant on scales comparable to the smallest dimensions of the observed prominence fine structures. We also show the ability of the 3D whole-prominence fine structure model to reveal the distribution of the prominence plasma with respect to its temperature within the prominence volume. This provides new insights into the composition of the prominence-corona transition region. We further demonstrate that the values of the plasma β are small throughout the majority of the modeled prominences when realistic photospheric magnetic flux distributions and prominence plasma parameters are assumed. While this is generally true, we also find that in the region with the deepest magnetic dips, the plasma β may increase towards unity. Finally, we show that the mass of the modeled prominence plasma is in good agreement with the mass of observed non-eruptive prominences.

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Plasma Structure and Dynamics

Cited by 16 publications

References 130 publications

FORWARD: A Toolset for Multiwavelength Coronal Magnetometry

FORWARD: A Toolset for Multiwavelength Coronal Magnetometry

Solar prominences: theory and models

Properties of the prominence magnetic field and plasma distributions as obtained from 3D whole-prominence fine structure modeling

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