Impulsive Near-relativistic Solar Electron Events: Delayed Injection with Respect to Solar Electromagnetic Emission

By D. Haggerty, E. Roelof. 2002

171 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/46dcf3c21b87e076ef3d1796ba1c4e091e0325c3

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In Astronomy and Astrophysics

1. D. Reames
2. Martin A. Lee
3. R. Schwenn
4. A. Tylka
5. E. Cliver
6. B. Tsurutani
7. Gary Zank
8. G. Lakhina

In Geophysics

1. D. Reames
2. E. Cliver
3. S. Kahler
4. R. Schwenn
5. David John McComas
6. Martin A. Lee
7. George Livadiotis
8. Nat Gopalswamy

Citations in the corpus

• Coronal Shocks and Solar Energetic Proton Events (2004, methodology): “From an examination of a sample of 80 38–315 keV beamlike electron events, Haggerty & Roelof (2002) obtained a median injection onset delay of 10 minutes from the flare impulsive phase.”
• Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation (2016, background): “These escaping impulsive SEPs sometimes propagate out to Earth-orbit without being scattered (see e.g., Mason et al. 1989; Haggerty and Roelof 2002).”
• A review of solar type III radio bursts (2014, background): “However, the injection time of energetic electrons at different energies does not correspond to the inferred injection time by looking at the associated type III bursts (Krucker et al., 1999; Haggerty & Roelof, 2002; Cane, 2003; Wang et al., 2006, 2011; Kahler et al., 2011; Klassen et al., 2012).”
• Shock Geometry, Seed Populations, and the Origin of Variable Elemental Composition at High Energies in Large Gradual Solar Particle Events (2005, background): “In order of increasing energy, the measurements come from the Ultra Low Energy Isotope Spectrometer (ULEIS; Mason et al. 1998) on the Advanced Composition Explorer (ACE ), the Electron, Proton, and Alpha Monitor (EPAM; Gold et al. 1998) on ACE, the Low Energy Matrix Telescope (LEMT) in the Energetic”
• A brief review of “solar flare effects” on the ionosphere (2009, background): “[29] What about relativistic electrons? Won’t they reach theEarthrapidlyandcontaminatetheflarephotoneffects? The acceleration of relativistic electrons at the flare site is often delayed from the flare by 5 to 15 min [Hudson et al. ,1 982; Haggerty and Roelof, 2002 ].”
• STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview (2008, unknown): “Recent work using energetic electron events and Type III radio bursts from WIND and ACE show that there is often a large temporal offset between a Type III burst, and the associated electron event (Krucker et al. 1999; Haggerty and Roelof 2002).”
• Space Weather: The Solar Perspective (2006, background): “) The delayed electrons come from coronal shocks, like the herringbones at type II radio bursts (Krucker et al., 1999; Klassen et al., 2002; Haggerty and Roelof, 2002).”
• Solar Flare Electron Spectra at the Sun and near the Earth (2007, background): “1); but most events are delayed, i.e., the≥20 keV electrons appear to be injected from 10 up to 30 minutes later (Krucker et al. 1999; Haggerty & Roelof 2002,\; Maia & Pick 2004; Klein et al. 2005).”