The dynamics of an erupting prominence

Klein, Karl‐Ludwig; Mouradian, Z.

doi:10.1051/0004-6361:20011513

Cited by 20 publications

(22 citation statements)

References 45 publications

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“…This is in accordance with the idea that moving type IV bursts are emitted by trapped suprathermal electrons, through either the gyrosynchrotron process or plasma emission, and that the radio sources are characterised by systematic outward motions, often in association with prominence eruptions (see, e.g. Klein & Mouradian 2002). .…”

Section: Radio and Hard X-ray Observationssupporting

confidence: 87%

Non-thermal processes associated with rising structures and waves during a “halo” type CME

Lehtinen¹,

Pohjolainen²,

Karlický

et al. 2005

A&A

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We analyse structures and events connected with a flare-associated "halo" type coronal mass ejection (CME) observed on December 18, 2000. A GOES C7.0 class X-ray flare started at 11:02 UT in NOAA Active Region 9269, located at N14 E03. Yohkoh SXT observed slowly rising soft X-ray loops already some 5 min before flare start. Hα images show a two-ribbon flare, remote brightenings, and a partly disappearing filament near the active region. A metric radio precursor was observed to start at 11:06:30 UT, simultaneously with impulsive emission in hard X-rays and microwaves. The frequency-drifting precursor envelope was superposed with J-and reverse drift bursts. The radio bursts traced large-scale soft X-ray loop structures about 160 000 km away from the flare core, and hard X-ray emission was observed at the ends of some of these loops. The precursor emission points to a rising structure where electron acceleration takes place. Later on, a radio type II burst (signature of a propagating shock, driven either by an ejecta or a blast wave) and an EIT wave were observed. We conclude that possible sources for the rising structure and accelerator of electron beams are (1) large-scale loops that connect the flare core region and the precursor site in the close vicinity of two separate rising filaments, and (2) a growing shock that accelerates electrons along closed field lines until the multipolar field is opened and the CME is lifted off. As neither X-ray nor EUV ejecta could be observed whether in the direction of the type II burst or near the radio precursor, we find some support for the shock wave scenario.

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Section: Radio and Hard X-ray Observationssupporting

confidence: 87%

Non-thermal processes associated with rising structures and waves during a “halo” type CME

Lehtinen¹,

Pohjolainen²,

Karlický

et al. 2005

A&A

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“…Since the flux rope moves outwards and expands, the internal thermal electron density decreases, and the plasma emission of the confined electrons occurs at gradually decreasing frequencies, as observed in the Type IV continuum during Episode 5. The moving radio source is often observed along the extrapolated trajectory of an erupting prominence (McLean 1973;Stewart et al 1978;MacQueen 1980;Kurokawa et al 1987;Klein & Mouradian 2002), so that one expects it to consist of dense plasma well within the CME structure as seen in white light, rather than near its front. Direct comparison of the radio source location with the CME confirms this view (Fig.…”

Section: An Interpretation Of Particle Acceleration During the Secondmentioning

confidence: 99%

The relativistic solar particle event of 2005 January 20: origin of delayed particle acceleration

Klein

Masson

Bouratzis

et al. 2014

A&A

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Context. The highest energies of solar energetic nucleons detected in space or through gamma-ray emission in the solar atmosphere are in the GeV range. Where and how the particles are accelerated is still controversial. Aims. We search for observational information on the location and nature of the acceleration region(s) by comparing the timing of relativistic protons detected on Earth and radiative signatures in the solar atmosphere during the particularly well-observed 2005 Jan. 20 event.Methods. This investigation focusses on the post-impulsive flare phase, where a second peak was observed in the relativistic proton time profile by neutron monitors. This time profile is compared in detail with UV imaging and radio spectrography over a broad frequency band from the low corona to interplanetary space. Results. It is shown that the late relativistic proton release to interplanetary space was accompanied by a distinct new episode of energy release and electron acceleration in the corona traced by the radio emission and by brightenings of UV kernels. These signatures are interpreted in terms of magnetic restructuring in the corona after the coronal mass ejection passage. Conclusions. We attribute the delayed relativistic proton acceleration to magnetic reconnection and possibly to turbulence in largescale coronal loops. While Type II radio emission was observed in the high corona, no evidence of a temporal relationship with the relativistic proton acceleration was found.

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“…A prominence may be heated during eruption and thus can brighten in emission (Filippov & Koutchmy 2002;Karlicky & Simberova 2002). Radio tracking of eruptive prominences show constant acceleration at heights solar radii (Klein & Mouradian 2002), and տ 0.5 92% of eruptive prominences were found to be associated with CMEs (Hori & Culhane 2002). Prominence plasma is only partially ionized and the draining of hydrogen lasts typically a day, much longer than for helium (Gilbert et al 2002).…”

Section: Filaments and Prominencesmentioning

confidence: 99%

Astrophysics in 2002

Trimble

Aschwanden

2003

PUBL ASTRON SOC PAC

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ABSTRACT. This has been the Year of the Baryon. Some low temperature ones were seen at high redshift, some high temperature ones were seen at low redshift, and some cooling ones were (probably) reheated. Astronomers saw the back of the Sun (which is also made of baryons), a possible solution to the problem of ejection of material by Type II supernovae (in which neutrinos push out baryons), the production of R Coronae Borealis stars (previously-owned baryons), and perhaps found the missing satellite galaxies (whose failing is that they have no baryons). A few questions were left unanswered for next year, and an attempt is made to discuss these as well.

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The dynamics of an erupting prominence

Cited by 20 publications

References 45 publications

Non-thermal processes associated with rising structures and waves during a “halo” type CME

Non-thermal processes associated with rising structures and waves during a “halo” type CME

The relativistic solar particle event of 2005 January 20: origin of delayed particle acceleration

Astrophysics in 2002

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