Magnetostatic structures of the solar corona. 2: The magnetic topology of quiescent prominences

Low, B. C.; Hundhausen, Joan R.

doi:10.1086/175572

Cited by 258 publications

(207 citation statements)

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“…Low and Hundhausen, 1995 here is only the sixth reported. This rarity suggests that prominence material is usually completely ionized during transit through the corona.…”

Section: By E/q Ratio Relative To the Proton Peak (E/q-l)mentioning

confidence: 77%

A prolonged He⁺ enhancement within a coronal mass ejection in the solar wind

Skoug¹,

Bame²,

Feldman³

et al. 1999

Geophysical Research Letters

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“…Low and Hundhausen, 1995 here is only the sixth reported. This rarity suggests that prominence material is usually completely ionized during transit through the corona.…”

Section: By E/q Ratio Relative To the Proton Peak (E/q-l)mentioning

confidence: 77%

A prolonged He⁺ enhancement within a coronal mass ejection in the solar wind

Skoug¹,

Bame²,

Feldman³

et al. 1999

Geophysical Research Letters

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“…Even in the quiescent phase, Filippov (1994) discovered a pattern typical of twisted flux tubes: a "fishbone" organization in Ha fibrils on both sides of the inversion line. Low and Hundhausen (1995) show how a twisted-flux tube topology can bring together many of the Ha and magnetic observations. Finally, the emergence of a twisted configuration is supported by recent vector field measurements (Leka et al 1996, Lites et al 1995.…”

Section: Prominence Supported In Twisted-flux Tubesmentioning

confidence: 90%

“…I then deduce that the latter should be realized in prominence feet; it is then natural that the feet are observed to form first (Martres et al 1966). Moreover, magnetic reconnection is required to progressively liberate the magnetic configuration from its deep anchorage (Low and Hundhausen 1995).…”

Section: Common Features Of Models With Dipsmentioning

confidence: 99%

Magnetic Fields in Filaments

Démoulin

1998

International Astronomical Union Colloquium

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Abstract. Filaments are present in highly non-potential magnetic configurations. On one hand, the complexity of modeling such 3-D configurations makes a useful comparison between observations and models difficult. On the other hand such highly sheared regions are more interesting and challenging for understanding eruptive phenomena like flares and coronal mass ejections. Fortunately, the presence of cold plasma allows us to measure the magnetic field inside prominences. Together with photospheric field measurements and other morphological observations, these provide a large set of puzzling constraints for plausible models of the magnetic configurations. Models are reviewed in the framework of present observational constraints with the aim to clarify a piece of the mystery which surrounds the magnetic configuration of filaments.

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“…closely related to filament eruptions [75], and it is generally believed that many filaments are supported by magnetic dips associated with a flux rope [76]. (4) Coronal cavities overlying a filament structure that are frequently observed to erupt as CMEs are considered to be the rope structures supporting the filaments [77].…”

Section: Energy Release Mechanisms Of Cmes: Mhd Studies With a Flux-rmentioning

confidence: 99%

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

Chen

2013

Chin. Sci. Bull.

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In this article I present a review of recent studies on coronal dynamics, including research progresses on the physics of coronal streamers that are the largest structure in the corona, physics of coronal mass ejections (CMEs) that may cause a global disturbance to the corona, as well as physics of CME-streamer interactions. The following topics will be discussed in depth: (1) acceleration of the slow wind flowing around the streamer considering the effect of magnetic flux tube curvature; (2) physical mechanism accounting for persistent releases of streamer blobs and diagnostic results on the temporal variability of the slow wind speed with such events; (3) force balance analysis and energy release mechanism of CMEs with a flux rope magnetohydrodynamic model; (4) statistical studies on magnetic islands along the coronal-ray structure behind a CME and the first observation of magnetic island coalescence with associated electron acceleration; and (5) white light and radio manifestations of CME-streamer interactions. These studies shed new light on the physics of coronal streamers, the acceleration of the slow wind, the physics of solar eruptions, the physics of magnetic reconnection and associated electron acceleration, the large-scale coronal wave phenomenon, as well as the physics accounting for CME shock-induced type II radio bursts. solar wind, coronal streamer, coronal mass ejection, solar radio burst, magnetic reconnection Citation:Chen Y. A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions.

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Magnetostatic structures of the solar corona. 2: The magnetic topology of quiescent prominences

Cited by 258 publications

References 0 publications

A prolonged He⁺ enhancement within a coronal mass ejection in the solar wind

A prolonged He⁺ enhancement within a coronal mass ejection in the solar wind

Magnetic Fields in Filaments

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

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Magnetostatic structures of the solar corona. 2: The magnetic topology of quiescent prominences

Cited by 258 publications

References 0 publications

A prolonged He+ enhancement within a coronal mass ejection in the solar wind

A prolonged He+ enhancement within a coronal mass ejection in the solar wind

Magnetic Fields in Filaments

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

Contact Info

Product

Resources

About

A prolonged He⁺ enhancement within a coronal mass ejection in the solar wind

A prolonged He⁺ enhancement within a coronal mass ejection in the solar wind