Reconnection Rate in the Decay Phase of a Long Duration Event Flare on 1997 May 12

Isobe, Hiroaki; Yokoyama, T.; Shimojo, Masataka; Morimoto, Taro; Kozu, H.; Eto, Shigeru; Narukage, Noriyuki; Shibata, Kazunari

doi:10.1086/324777

Cited by 107 publications

(103 citation statements)

References 39 publications

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“…The method for calculating the reconnection rate outlined by Isobe et al (2002), derives the temperature T and the emission measure using the filter ratio method on SXT data. As this was not possible with this current data set, it is assumed that we have a temperature of 1.0 MK (peak formation temperature of 171 Å) and a density n of 3.0 × 10 9 cm −3 (Isobe et al 2002; Ramesh et al 2005).…”

Section: Estimation Of Reconnection Ratementioning

confidence: 99%

“…As this was not possible with this current data set, it is assumed that we have a temperature of 1.0 MK (peak formation temperature of 171 Å) and a density n of 3.0 × 10 9 cm −3 (Isobe et al 2002; Ramesh et al 2005). The effect of varying these values is discussed later.…”

Section: Estimation Of Reconnection Ratementioning

confidence: 99%

“…where the volume of the arcade V is given by the area taken up by the flare loops on the image A r times the line-of-sight length l. We have assumed for this that A r was equal to the number of pixels on the EUV image that had an intensity greater than 0.2 of the maximum intensity, as in Isobe et al (2002). Also as a first approximation, it is taken that the line-of-sight l is equal to the distance between the footpoints of the arcade.…”

Section: Estimation Of Reconnection Ratementioning

confidence: 99%

“…Flare loop arcades have been studied extensively from either theoretical (Sturrock 1968;Kopp & Pneuman 1976;Yokoyama & Shibata 1998) or observational (McKenzie & Hudson 1999;Yokoyama et al 2001;Isobe et al 2002) perspectives or both (Forbes & Acton 1996). There are various models for the magnetic reconnection process itself which differ in their estimation of the reconnection rate in two spatial dimensions (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Firstly, Isobe et al (2002) uses Yohkoh Soft X-ray Telescope (SXT) data with the corresponding photospheric magnetogram taken with the Solar and Heliospheric Observatory using the Michelson Doppler Imager (SOHO/MDI) to analyse the decay phase of a long duration event (LDE) flare on the disc. They find the energy release rate in the decay phase to be ten times lower than in the rise phase and derive a magnetic reconnection rate of 0.001−0.01.…”

Section: Introductionmentioning

confidence: 99%

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Indirect calculation of the magnetic reconnection rate from flare loops

Noglik¹,

Walsh²,

Ireland

2005

A&A

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Abstract. High time resolution Transition Region And Coronal Explorer (TRACE) 171 and 195 Å observations of the evolution of flare loops on 1999 March 18 have been investigated. Given the location of the magnetic loops on the northeast solar limb and the cadence of the TRACE observations (∼50 s), an estimation of the footpoint velocity due to ongoing reconnection was undertaken. This was achieved by calculating the velocity at which successive loops brighten in the emission lines during the postflare phase. A typical footpoint velocity of 1.5 km s −1 ± 0.7 km s −1 is obtained and a reconnection rate of ∼0.001−0.03 is determined using the method outlined in Isobe et al. (2002, ApJ, 566, 528). This value for the reconnection rate is consistent with the regime outlined by Petschek's model for magnetic reconnection.

show abstract

Section: Estimation Of Reconnection Ratementioning

confidence: 99%

Section: Estimation Of Reconnection Ratementioning

confidence: 99%

Section: Estimation Of Reconnection Ratementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Indirect calculation of the magnetic reconnection rate from flare loops

Noglik¹,

Walsh²,

Ireland

2005

A&A

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show abstract

An Observational Overview of Solar Flares

Fletcher¹,

Dennis²,

Hudson³

et al. 2011

High-Energy Aspects of Solar Flares

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We present an overview of solar flares and associated phenomena, drawing upon a wide range of observational data primarily from the RHESSI era. Following an introductory discussion and overview of the status of observational capabilities, the article is split into topical sections which deal with different areas of flare phenomena (footpoints and ribbons, coronal sources, relationship to coronal mass ejections) and their interconnections. We also discuss flare soft X-ray spectroscopy and the energetics of the process. The emphasis is to describe the observations from multiple points of view, while bearing in mind the models that link them to each other and to theory. The present theoretical and observational understanding of solar flares is far from complete, so we conclude with a brief discussion of models, and a list of missing but important observations.

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Magnetic Reconnection for Coronal Conditions: Reconnection Rates, Secondary Islands and Onset

Cassak¹,

Shay²

2011

Space Sciences Series of ISSI

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Reconnection Rate in the Decay Phase of a Long Duration Event Flare on 1997 May 12

Cited by 107 publications

References 39 publications

Indirect calculation of the magnetic reconnection rate from flare loops

Indirect calculation of the magnetic reconnection rate from flare loops

An Observational Overview of Solar Flares

Magnetic Reconnection for Coronal Conditions: Reconnection Rates, Secondary Islands and Onset

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