The eruptive events on September 30, 1998: 1. The jet

Bagalá, L. G.; Stenborg, Guillermo; Schwenn, R.; Haerendel, G.

doi:10.1029/2000ja004017

Cited by 7 publications

(2 citation statements)

References 9 publications

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“…Jets in Hα, the Fe XIV (green) line and soft X-rays were seen in this structure between roughly 13:15 and 13:30 UT, i.e. during the moving radio emission, by Bagalá et al (2001) who give a detailed discussion of the coronal evolution during the event (cf. also Maia & Pick 2004).…”

Section: A22 1997 September 20: Electron Release Associated With Amentioning

confidence: 99%

Coronal phenomena at the release of solar energetic electron events

Klein¹,

Krucker²,

Trottet³

et al. 2005

A&A

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Abstract. We investigate dynamical processes in the solar corona at the release of electrons (∼30−500 keV) detected by the Wind/3DP experiment, with the aim to clarify the relationship between coronal acceleration and the escape of electrons to interplanetary space. Energetic electrons and plasma in the corona are traced using radio, EUV and X-ray observations. 40 events were identified where the release time of the electrons could be determined within an uncertainty of a few minutes and occurred during the observing hours of the Nançay Radioheliograph. All were accompanied by decametric-to-kilometric type III bursts (Wind/WAVES), and 30 by metric radio emission in the western hemisphere. The main findings from these 30 events are: (i) Electrons detected at Wind are released at the time of distinct episodes of electron acceleration in the corona signalled by radio emission. The release may occur at the start of the radio event or up to an hour later. (ii) The most conspicuous examples of delayed electron release occur in events associated with complex, long lasting (>10 min, up to seveal hours) radio emission. Radio observations suggest that in these cases the earlier accelerated electrons remain confined in the corona or are injected into flux tubes which are not connected to the spacecraft. (iii) Type II bursts revealing shock waves in the corona accompany about a third of the events. But the shock waves occur in general together with type IV radio signatures due to long lasting acceleration not related to the shock. With a few exceptions these type IV emissions have a clearer timing relationship with the electron release to space than the type II bursts. We conclude that the combination of time-extended acceleration at heights 0.5 R above the photosphere with the injection of electrons into a variety of closed and open magnetic field structures explains the broad variety of timing shown by the radio observations and the in situ measurements.

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Section: A22 1997 September 20: Electron Release Associated With Amentioning

confidence: 99%

Coronal phenomena at the release of solar energetic electron events

Klein¹,

Krucker²,

Trottet³

et al. 2005

A&A

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“…From fast-time-cadence radio imaging observations in the metric domain it is now known that the sites of radio emission tend to follow the latitudinal extent of the coronal mass ejection later seen in coronagraphic images (Maia et al 1999). The time-scales involved in the magnetic restructuring in the early development of the CME are of the order of a few minutes and may involve magnetic flux systems quite far from the main flaring region (Maia et al 2001;Delannée et al 2000;Aulanier et al 1998;Bagalá et al 2001;.…”

Section: Introductionmentioning

confidence: 99%

Interpretation of a complex CME event: Coupling of scales in multiple flux systems

Maia

Aulanier

Wang

et al. 2003

A&A

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Abstract. Using multi-wavelength observations, in particular in imagery, recorded by SOHO/LASCO-MDI, Yohkoh/SXT, the Meudon spectroheliograph and the Nançay radioheliograph, and performing a linear force-free field extrapolation, we analyzed the triggering and the development of a complex eruptive event in the chromosphere and in the corona. This event included an X1 class flare and an eruptive filament within an active region, but it also involved a whole active complex spanning over 40 degrees of heliolongitude. It resulted in a fast and decelerating partial halo CME, associated with a Moreton wave and a complex series of metric, decimetric and microwave radio bursts. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources give strong arguments in favor of the generalized breakout model for the triggering of the eruption. The observations are consistent with the occurrence of magnetic reconnection at the null point three minutes before the start of the eruption, which is consistent with other observed CME precursors. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME, and that secondary reconnections at low altitude probably occurred remotely in the active complex. Our results show that the triggering and evolution of this complex CME involved multiple magnetic flux systems over a large coronal volume surrounding the flare site, and that it resulted from the coupling of scales from narrow reconnection current sheets to very large inter active region magnetic connections.

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