A survey of soft X-ray limb flare images - The relation between their structure in the corona and other physical parameters

Pallavicini, R.; Serio, S.; Vaiana, G. S.

doi:10.1086/155452

Cited by 291 publications

(114 citation statements)

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“…Recently Cane, McGuire, and von Rosenvinge [1986] have related the two acceleration phases to two classes of solar flare particle eventswhich can be distinguished by a variety of signaturesincluding the duration of their associated soft X-ray emission [Pallavicini, Serio, and Vaiana, 1977]. The first class, characterized by short duration impulsive events, is probably due to impulsive energy release in compact source regions relatively low in the corona.…”

Section: B Trapping and Escape Of Particles And Multiple Acceleratiomentioning

confidence: 99%

Particle acceleration in solar flares

Mandzhavidze

Ramaty

1993

Nuclear Physics B - Proceedings Supplements

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Section: B Trapping and Escape Of Particles And Multiple Acceleratiomentioning

confidence: 99%

Particle acceleration in solar flares

Mandzhavidze

Ramaty

1993

Nuclear Physics B - Proceedings Supplements

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“…Based on solar radio bursts, Wild et al [1963] suggested that electrons are accelerated to produce type III radio bursts, and protons are accelerated at shock waves seen as type II bursts, although both radiations are emitted by electrons. These two sources were later classified into impulsive and "long-enduring," soft X-ray events by Pallavicini et al [1977]. Recently Reames [2013] reviewed the two physical mechanisms involved in the acceleration of SPEs or solar energetic particles (SEPs).…”

Section: Introductionmentioning

confidence: 99%

Characteristics of four SPE groups with different origins and acceleration processes

et al. 2015

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Solar proton events (SPEs) can be categorized into four groups based on their associations with flare or CME inferred from onset timings as well as acceleration patterns using multienergy observations. In this study, we have investigated whether there are any typical characteristics of associated events and acceleration sites in each group using 42 SPEs from 1997 to 2012. We find the following: (i) if the proton acceleration starts from a lower energy, a SPE has a higher chance to be a strong event (> 5000 particle flux per unit (pfu)) even if its associated flare and/or CME are not so strong. The only difference between the SPEs associated with flare and CME is the location of the acceleration site. (ii) For the former (Group A), the sites are very low (∼ 1 Rs) and close to the western limb, while the latter (Group C) have relatively higher (mean = 6.05 Rs) and wider acceleration sites. (iii) When the proton acceleration starts from the higher energy (Group B), a SPE tends to be a relatively weak event (< 1000 pfu), although its associated CME is relatively stronger than previous groups. (iv) The SPEs categorized by the simultaneous acceleration in whole energy range within 10 min (Group D) tend to show the weakest proton flux (mean = 327 pfu) in spite of strong associated eruptions. Based on those results, we suggest that the different characteristics of SPEs are mainly due to the different conditions of magnetic connectivity and particle density, which are changed with longitude and height as well as their origin.

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“…There were no other important flare except the X5.7 during 14-16, July 2000. Based on the flare classification given by Pallavicini et al (1977), the flare X5.7 was a gradual flare. While the whole duration of the flare is shorter than 1 hour, so the flare belonged to impulsive flare based on the definition of a flare by its time structure.…”

Section: Discussionmentioning

confidence: 99%

Analysis of the Acceleration Process of SEPs by an Interplanetary Shock for Bastille Day Event

Han

2004

Proc. IAU

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Abstract. Based on the solar energetic particle (SEP) data from ACE and GOES satellites, the acceleration of SEP by CME-driven shock in interplanetary space was investigated. The results showed that the acceleration process of SEP by the Bastille CME-driven shock ran through the whole space from the sun to the magnetosphere. The highest energy of SEP accelerated by the shock was greater than 100MeV. A magnetic bottle associated with the CME captured a lot of high energy particles with some of them having energy greater than 100MeV. Based on magnetic field data of solar wind observed by ACE data, we found that the the magnetic bottle associated with the Bastille CME was the sheath caused by the CME in fact.

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A survey of soft X-ray limb flare images - The relation between their structure in the corona and other physical parameters

Cited by 291 publications

References 0 publications

Particle acceleration in solar flares

Particle acceleration in solar flares

Characteristics of four SPE groups with different origins and acceleration processes

Analysis of the Acceleration Process of SEPs by an Interplanetary Shock for Bastille Day Event

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