Energetic Neutrons, Protons, and Gamma Rays during the 1990 May 24 Solar Cosmic‐Ray Event

Debrunner, H.; Lockwood, J. A.; Barat, C.; Bütikofer, R.; Dezalay, J. P.; Flückiger, E. O.; Кузнецов, А. В.; Ryan, J. M.; Sunyaev, R.; Terekhov, O.; Trottet, G.; Vilmer, Nicole

doi:10.1086/303895

Cited by 77 publications

(66 citation statements)

References 22 publications

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“…The acceleration processes in the flaring active region clearly supplied particles to the low solar atmosphere, but not the relativistic protons detected at Earth. The lack of energetic charged particle injection into space during the main hard X-ray or gamma-ray emission was reported for other particle events at subrelativistic (Kallenrode & Wibberenz 1991;Laitinen et al 2000) and relativistic (Debrunner et al 1997;Klein et al 1999) energies.…”

Section: Discussionmentioning

confidence: 74%

“…We thereby pursue the study of individual solar relativistic proton events (called ground level events, GLEs) which suggested that relativistic protons are injected into interplanetary space well after the production of interacting energetic particles revealed by their gamma-ray and hard X-ray emission, but in time coincidence with acceleration in the middle corona (∼0.1-1 R above the photosphere, say) that shows up in decimetric and metric radio emission (Klein et al 1999;Klein & Trottet 2001). While the delay of relativistic proton injection with respect to hard X-ray, gamma-ray and microwave signatures of mildly relativistic electrons and suprathermal protons in the low solar atmosphere was known earlier (e.g., Carmichael 1962;Cliver et al 1982;Kahler 1994;Debrunner et al 1997), the connection with signatures of coronal particle acceleration at greater height, where collisional radiative signatures are inefficient due to the low ambient density, and gyrosynchrotron emission is faint because of the weak magnetic field, has only rarely been investigated (Palmer & Smerd 1972;Kocharov et al 1994;Akimov et al 1996;Klein et al 1999;Miroshnichenko et al 2000).…”

Section: Introductionmentioning

confidence: 90%

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Coronal electron acceleration and relativistic proton production during the 14 July 2000 flare and CME

Klein

Trottet

Lantos

et al. 2001

A&A

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Abstract. The large solar flare of 14 July 2000 10 UT occurred in an active region near the central meridian. It was accompanied by the eruption of a filament and a rapid halo-type coronal mass ejection (CME). Large particle fluxes were detected up to relativistic energies at 1 AU. In this paper accelerated particles and plasma structures in the corona are traced using radio, X-ray, EUV and visible light observations, together with neutron monitor measurements of relativistic protons at 1 AU. Both the bulk of the radio emission at decimetric and longer waves and the escape of suprathermal electrons and relativistic protons from the Sun were delayed by 10-20 min with respect to the hard X-ray emission. Despite the delay and the association with a flare near the central meridian the neutron monitor time profile was impulsive. We show that the escape of the relativistic protons occurred in time coincident both with a coronal shock wave, which may be the bow shock of the CME, and with radio sources which trace electron acceleration and magnetic field reconfiguration in the western hemisphere. Three observations support the idea that the relativistic protons were accelerated during this reconfiguration, at heights between 0.1 and 1 R above the photosphere, and not in the flaring active region or at the bow shock of the CME: (i) the rise of the neutron monitor count rates is simultaneous with the brightening of a new continuum radio source; (ii) the duration of the continuum emission is similar to the rise time of the neutron monitor count rates; (iii) the radio source is close to the Earth-connected interplanetary magnetic field line.

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Section: Discussionmentioning

confidence: 74%

Section: Introductionmentioning

confidence: 90%

Coronal electron acceleration and relativistic proton production during the 14 July 2000 flare and CME

Klein

Trottet

Lantos

et al. 2001

A&A

Self Cite

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“…Besides prominent microwave ) and hard X-ray (HXR; Pelaez et al 1992) emission, this renowned X9/1B flare simultaneously produced energetic neutrons, protons, and γ -rays, and has since been studied extensively (Shea et al 1991;Debrunner et al 1992Debrunner et al , 1993Debrunner et al , 1997Kocharov et al 1994Kocharov et al , 1996Torsti et al 1996;Vilmer et al 2003). The γ -ray lightcurve up to 95 MeV measured by the PHEBUS detector on the GRANAT spacecraft shows two peaks at 20:48:12 and 20:48:36 UT, respectively (Debrunner et al 1997).…”

Section: Observation and Analysismentioning

confidence: 99%

Observation of a Moreton Wave and Wave-Filament Interactions Associated With the Renowned X9 Flare on 1990 May 24

Liu

et al. 2013

ApJ

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Using Big Bear Solar Observatory film data recently digitized at NJIT, we investigate a Moreton wave associated with an X9 flare on 1990 May 24, as well as its interactions with four filaments F1-F4 located close to the flaring region. The interaction yields interesting insight into physical properties of both the wave and the filaments. The first clear Moreton wavefront appears at the flaring-region periphery at approximately the same time as the peak of a microwave burst and the first of two γ -ray peaks. The wavefront propagates at different speeds ranging from 1500-2600 km s −1 in different directions, reaching as far as 600 Mm away from the flaring site. Sequential chromospheric brightenings are observed ahead of the Moreton wavefront. A slower diffuse front at 300-600 km s −1 is observed to trail the fast Moreton wavefront about one minute after the onset. The Moreton wave decelerates to ∼550 km s −1 as it sweeps through F1. The wave passage results in F1's oscillation which is featured by ∼1 mHz signals with coherent Fourier phases over the filament, the activation of F3 and F4 followed by gradual recovery, but no disturbance in F2. Different height and magnetic environment together may account for the distinct responses of the filaments to the wave passage. The wavefront bulges at F4, whose spine is oriented perpendicular to the upcoming wavefront. The deformation of the wavefront is suggested to be due to both the forward inclination of the wavefront and the enhancement of the local Alfvén speed within the filament channel.

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“…In a study of several events of the SMM era, Ramaty and coworkers [120] found an event-to-event variation of the ratio of protons at energies above 30 MeV inferred from gamma-ray modelling and from in situ measurements in a broad range between about 0.01 and 100 (see also [40]). The number of protons above 30 MeV in the large SEP event on 1990 May 24 was found to be smaller than the number of protons interacting in the low solar atmosphere [30]. For electrons in the energy range between a few tens of keV and a few MeV the situation is different: the number of electrons detected in space is always found to be orders of magnitude smaller than the number required for hard X-ray emission by collisional bremsstrahlung, although a correlation seems to exist between the energy spectra of the two populations [120,38,87].…”

Section: 4mentioning

confidence: 77%

The acceleration and propagation of solar energetic particles

Dalla

2004

AIP Conference Proceedings

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Solar Energetic Particles (SEPs) are an important component of Space Weather, including radiation hazard to humans and electronic equipment, and the ionisation of the Earth's atmosphere. We review the key observations of SEPs, our current understanding of their acceleration and transport, and discuss how this knowledge is incorporated within Space Weather forecasting tools. Mechanisms for acceleration during solar flares and at shocks driven by Coronal Mass Ejections are discussed, as well as the timing relationships between signatures of solar eruptive events and the detection of SEPs in interplanetary space. Evidence on how the parameters of SEP events are related to those of the parent solar activity is reviewed and transport effects influencing SEP propagation to near-Earth locations are examined. Finally, the approaches to forecasting Space Weather SEP effects are discussed. We conclude that both flare and CME shock acceleration contribute to Space Weather relevant SEP populations and need to be considered within forecasting tools.

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Energetic Neutrons, Protons, and Gamma Rays during the 1990 May 24 Solar Cosmic‐Ray Event

Cited by 77 publications

References 22 publications

Coronal electron acceleration and relativistic proton production during the 14 July 2000 flare and CME

Coronal electron acceleration and relativistic proton production during the 14 July 2000 flare and CME

Observation of a Moreton Wave and Wave-Filament Interactions Associated With the Renowned X9 Flare on 1990 May 24

The acceleration and propagation of solar energetic particles

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