Physics of Solar Prominences: II—Magnetic Structure and Dynamics

Mackay, D. H.; Karpen, J. T.; Ballester, J. L.; Schmieder, B.; Aulanier, G.

doi:10.1007/s11214-010-9628-0

Cited by 586 publications

(603 citation statements)

References 248 publications

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“…The erupting prominence is invariably seen to be more highly twisted than before it erupted (e.g. Mackay et al, 2010;Mackay and Yeates, 2012). Furthermore, three-dimensional (3D) reconnection naturally tends to create twist (Berger and Field, 1984;Hornig and Priest, 2003;Priest, Longcope, and Janvier, 2016).…”

Section: Introductionmentioning

confidence: 99%

Flux Rope Formation Due to Shearing and Zipper Reconnection

2018

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Zipper reconnection has been proposed as a mechanism for creating most of the twist in the flux tubes that are present prior to eruptive flares and coronal mass ejections. We have conducted a first numerical experiment on this new regime of reconnection, where two initially untwisted parallel flux tubes are sheared and reconnected to form a large flux rope. We describe the properties of this experiment, including the linkage of magnetic flux between concentrated flux sources at the base of the simulation, the twist of the newly formed flux rope, and the conversion of mutual magnetic helicity in the sheared pre-reconnection state into the self-helicity of the newly formed flux rope.

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Section: Introductionmentioning

confidence: 99%

Flux Rope Formation Due to Shearing and Zipper Reconnection

2018

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“…Prominences, also referred to as filaments when observed against the solar disk, are cool, dense, magnetized formations of 10 4 K plasma embedded in the 10 6 K solar corona (for reviews see Mackay et al 2010;Labrosse et al 2010). They are located above polarity inversion lines (PILs or filament channels), i.e., the line that divides regions of opposite magnetic flux in the photosphere.…”

Section: Introductionmentioning

confidence: 99%

The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet

Suárez

Ramos

Bueno

2014

A&A

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Context. Determining the magnetic field vector in quiescent solar prominences is possible by interpreting the Hanle and Zeeman effects in spectral lines. However, observational measurements are scarce and lack high spatial resolution. Aims. We determine the magnetic field vector configuration along a quiescent solar prominence by interpreting spectropolarimetric Results. For the most probable magnetic field vector configuration, the analysis depicts a mean field strength of 7 gauss. We do not find local variations in the field strength except that the field is, on average, lower in the prominence body than in the prominence feet, where the field strength reaches ∼25 gauss. The averaged magnetic field inclination with respect to the local vertical is ∼77 • . The acute angle of the magnetic field vector with the prominence main axis is 24 • for the sinistral chirality case and 58 • for the dextral chirality. These inferences are in rough agreement with previous results obtained from the analysis of data acquired with lower spatial resolutions.

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“…It is known that there is a variety of solar prominences having maximum heights in the range 30-50 thousand kilometers (Mackay et al 2010 and references therein). It means that comet impact-generated photospheric mass ejections can form a certain type of solar/stellar prominences, too.…”

Section: Impulse Aerodynamic Deceleration Of Crushed Comet Nuclei In mentioning

confidence: 99%

Stellar ejecta from falling comet-like bodies: young stars

Ibodov

Ibadov

2013

Proc. IAU

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High-resolution spectral observations of young stars with dense protoplanetary discs like Beta Pictoris led to the discovery of variable emission lines of metal atoms, Na, Fe etc., that indicate the presence of fluxes of comet-like evaporating bodies falling onto the stars, FEBs. Assuming the presence of stellar atmospheres similar to the solar one, we show that passages of the FEBs through the stellar chromosphere and photosphere with velocities around 600 km/s will be accompanied by aerodynamic crushing of the nuclei, transverse expansion of the crushed matter, “explosion” of the flattened nuclei in a relatively very thin sub-photosphere layer due to sharp deceleration, and impulse production of a hot plasma. The impulsive rise of the layer's temperature and density lead to the generation of a strong “blast” shock wave and shock wave-induced ejection/eruption of hot plasma into space above the chromosphere. Observations of such impact-induced high-temperature phenomena are of interest for the physics/prognosis of stellar/solar flares as well as physics of comets.

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Physics of Solar Prominences: II—Magnetic Structure and Dynamics

Cited by 586 publications

References 248 publications

Flux Rope Formation Due to Shearing and Zipper Reconnection

Flux Rope Formation Due to Shearing and Zipper Reconnection

The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet

Stellar ejecta from falling comet-like bodies: young stars

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