<i>Wind</i>Spacecraft Observations of Solar Impulsive Electron Events Associated with Solar Type III Radio Bursts

Ergun, R. E.; Larson, D. E.; Lin, R. P.; McFadden, J. P.; Carlson, C. W.; Anderson, K. A.; Muschietti, L.; McCarthy, Michael; Parks, G. K.; Rème, H.; Bosqued, J. M.; d’Uston, C.; Sanderson, T. R.; Wenzel, K.‐P.; Kaiser, M. L.; Lepping, R. P.; Bale, S. D.; Kellogg, P. J.; Bougeret, J. L.

doi:10.1086/305954

Cited by 204 publications

(146 citation statements)

References 29 publications

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“…1a). These suggest that lowenergy electrons are responsible for the generation of type III radio emissions, which is consistent with previous studies of impulsive electron injections (Wang et al 2006b) and in situ Langmuir waves (e.g., Ergun et al 1998). Based on simulations, Kontar & Reid (2009) suggest that solar impulsive electrons are injected simultaneously at all energies at the Sun, but the lowenergy electrons are significantly decelerated by beam-plasma interactions in the IPM, to produce the inferred earlier injection before high-energy electrons.…”

Section: Summary and Discussionsupporting

confidence: 88%

The injection of ten electron/³He-rich SEP events

Wang¹,

Krucker

Mason

et al. 2016

A&A

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We have derived the particle injections at the Sun for ten good electron/ 3 He-rich solar energetic particle (SEP) events, using a 1.2 AU particle path length (suggested by analysis of the velocity dispersion). The inferred solar injections of high-energy (∼10 to 300 keV) electrons and of ∼MeV/nucleon ions (carbon and heavier) start with a delay of 17 ± 3 min and 75 ± 14 min, respectively, after the injection of low-energy (∼0.4 to 9 keV) electrons. The injection duration (averaged over energy) ranges from ∼200 to 550 min for ions, from ∼90 to 160 min for low-energy electrons, and from ∼10 to 30 min for high-energy electrons. Most of the selected events have no reported Hα flares or GOES SXR bursts, but all have type III radio bursts that typically start after the onset of a low-energy electron injection. All nine events with SOHO/LASCO coverage have a relatively fast (>570 km s −1 ), mostly narrow ( 30 • ), west-limb coronal mass ejection (CME) that launches near the start of the low-energy electron injection, and reaches an average altitude of ∼1.0 and 4.7 R S , respectively, at the start of the high-energy electron injection and of the ion injection. The electron energy spectra show a continuous power law extending across the transition from low to high energies, suggesting that the low-energy electron injection may provide seed electrons for the delayed high-energy electron acceleration. The delayed ion injections and high ionization states may suggest an ion acceleration along the lower altitude flanks, rather than at the nose of the CMEs.

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Section: Summary and Discussionsupporting

confidence: 88%

The injection of ten electron/³He-rich SEP events

Wang¹,

Krucker

Mason

et al. 2016

A&A

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“…Therefore, low-energy ( < ∼ 13 keV) electrons accelerated by the C6.6 flare can easily escape from the low corona to interplanetary space and generate the prominent type III radio bursts. This agrees with the Langmuir waves that scatter to produce the type III radio emission that were observed simultaneously with the arrival of ∼2-10 keV electrons at 1 AU (Ergun et al 1998). The open field lines are well connected to the IMF lines that connect the Sun with the Earth, facilitating electrons to quickly reach the spacecraft.…”

Section: Solar Observations and Coronal Magnetic Topologiessupporting

confidence: 81%

Coronal magnetic topology and the production of solar impulsive energetic electrons

Sun

Wang

et al. 2013

A&A

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We investigate two candidate solar sources or active regions (ARs) in association with a solar impulsive energetic electron (SIEE) event on 2002 October 20. The solar particle release (SPR) times of SIEEs are derived by using their velocity dispersion with consideration of the instrumental effect. It is found that there are double electron injections at the Sun. The low-energy ( < ∼ 13 keV) electron injection coincides with a C6.6 flare in AR10154 and is accompanied with prominent type III radio bursts rather than a stronger M1.8 flare in AR10160. The M1.8 flare produces, however, faint type III radio bursts. Electrons of ∼25 to ∼300 keV are released ∼9 min later when a jet-like CME travels to ∼2.6 solar radii. We further examine the coronal magnetic configurations above the two ARs based on the potential field source surface (PFSS) model. It is found that open field lines, rooted in AR10154 and well connected to the Earth, provide escaping channels for energetic electrons. Only a small portion of magnetic fields are opened above AR10160, being responsible for the faint type III radio bursts. These lines are, however, not well connected, making it impossible for SIEEs detection by near-Earth spacecraft. The results appear to establish a physical link between coronal magnetic topology, formation of type III radio bursts, and production of SIEEs.

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“…The event selection criteria and a brief description of the 3DP instrument and data reduction are given in Ergun et al (1998) and in Krucker et al (1999). We selected events from two previously posted lists: the period 15 November 1994 to 22 June 2001, and a second period coinciding with the observations by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI) from February 2002 to October 2002.…”

Section: Selection Of the Impulsive Near-relativistic Electron Eventsmentioning

confidence: 99%

The Production of Near-Relativistic Electrons by CME-Driven Shocks

Kahler¹,

Auraß

Mann

et al. 2004

Proc. IAU

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Abstract. The solar sources of near-relativistic (E >30 keV) electron events observed at 1 AU are poorly understood. In general, the solar injection times deduced from the observed 1 AU onset times and assumed 1.2 AU travel distances yield injection times about 10 minutes after the associated flare impulsive phases and type III radio burst times. One interpretation is that the apparent delays occur in the interplanetary medium, probably due to scattering of the electrons. If the injection times are delayed from the impulsive phases, the electron acceleration might take place in CME-driven shocks. Here a large number of electron events observed with the UC/Berkeley 3DP detector on the Wind spacecraft are compared with CMEs observed by the Lasco coronagraph on SOHO and with type II bursts observed by the 40 to 800 MHz radio receiver at the Astrophysikalisches Institut Potsdam (AIP) and by the 20 kHz to 14 MHz WAVES instrument on the Wind spacecraft. The acceleration of at least some of the electron events is not consistent with the shock hypothesis.

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WindSpacecraft Observations of Solar Impulsive Electron Events Associated with Solar Type III Radio Bursts

Cited by 204 publications

References 29 publications

The injection of ten electron/³He-rich SEP events

The injection of ten electron/³He-rich SEP events

Coronal magnetic topology and the production of solar impulsive energetic electrons

The Production of Near-Relativistic Electrons by CME-Driven Shocks

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WindSpacecraft Observations of Solar Impulsive Electron Events Associated with Solar Type III Radio Bursts

Cited by 204 publications

References 29 publications

The injection of ten electron/3He-rich SEP events

The injection of ten electron/3He-rich SEP events

Coronal magnetic topology and the production of solar impulsive energetic electrons

The Production of Near-Relativistic Electrons by CME-Driven Shocks

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Product

Resources

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The injection of ten electron/³He-rich SEP events

The injection of ten electron/³He-rich SEP events