Proton, helium, and electron spectra during the large solar particle events of October-November 2003

By R. Mewaldt, C. Cohen, A. Labrador, R. Leske, G. Mason, M. Desai, M. Looper, J. Mazur, R. Selesnick, D. Haggerty. 2005

203 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/81f5e12957f877e1cc3b886a4891f497fbd15395

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In Astronomy and Astrophysics

1. H. Hudson
2. A. Posner
3. S. Krucker
4. A. Emslie
5. Brian R. Dennis
6. L. Fletcher
7. L. Sui
8. M. Temmer

Citations in the corpus

• A Model for Spectral and Compositional Variability at High Energies in Large, Gradual Solar Particle Events (2006, unknown): “…), the Solar and Heliospheric Observatory (SOHO), and other satellites in cycle 23 (Cane et al. 2003; Cohen et al. 1999a, 1999b, 2003, 2005; Mäkelä & Torsti 2001; Mewaldt et al. 2005; Reames et al. 2001; Reames & Ng 2004; Torsti et al. 2000; Tylka 2001; Tylka et al. 2000, 2001, 2002, 2005, 2006).”
• Up to 1‐hour forecasting of radiation hazards from solar energetic ion events with relativistic electrons (2007, methodology): “Pending better techniques to come, an in situ warning system for the Earth-Moon system that measures relativistic electrons should be required for all non-LEO human missions [e.g., Cohen et al., 2001; Miroshnichenko 2005].”
• GLOBAL ENERGETICS OF THIRTY-EIGHT LARGE SOLAR ERUPTIVE EVENTS (2012, methodology): “A similar approach was followed in analyzing the “Halloween” events (Mewaldt et al. 2005) and in a subsequent survey of 17 events (Mewaldt 2006).”
• Heavy-Ion Elemental Abundances in Large Solar Energetic Particle Events and Their Implications for the Seed Population (2006, background): “…processes similar to those occurring during IP shock events (see Desai et al. 2004), thus causing the energy spectra to exhibit species-dependent breaks between 1 and 10 MeV nucleon 1 (e.g., Mewaldt et al. 2005b, 2005a; Cohen et al. 2005) and the Fe/O ratios to decrease with increasing energy.”
• Hard X-ray emission from the solar corona (2008, background): “We note that the fraction of flare energy that eventually appears in particles accelerated by the CME-driven shock may be large (of order 10 %; see Emslie et al 2005; Mewaldt et al 2005).”