Abundances of Heavy and Ultraheavy Ions in 3He-rich Solar Flares

By G. Mason, J. Mazur, Jason R Dwyer, J. Jokipii, R. Gold, S. Krimigis. 2004

158 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f32e6e767634e4099ef1c9974f4f83fafb2a0181

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In Astronomy and Astrophysics

1. D. Reames
2. Martin A. Lee
3. A. Tylka
4. A. Posner
5. C. Cohen
6. R. Mewaldt
7. G. Mason
8. C. Ng

Citations in the corpus

• A Model for Spectral and Compositional Variability at High Energies in Large, Gradual Solar Particle Events (2006, background): “…adopt theoretical charge-state distributions for flare ions corresponding to the temperature TCare ¼ 4:0 MK; Reames et al. (1994) found that temperatures of 3Y5MK yieldmeanQ/A values that roughly organize the abundance patterns in impulsive events (Reames & Ng 2004;Mason et al. 2004; see also Fig.”
• Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation (2016, unknown): “8 right panel, taken from Mason et al. (2004).”
• A Unified Picture of the First Ionization Potential and Inverse First Ionization Potential Effects (2004, background): “Some FIP selectivity is evident around atomic masses corresponding to Kr, Rb, Sr, etc., in recent observations of SEP ultraheavy ions in impulsive solar flares (Mason et al. 2004, their Fig.”
• Heavy-Ion Elemental Abundances in Large Solar Energetic Particle Events and Their Implications for the Seed Population (2006, methodology): “In order to identify the source populations for LSEP events, we compare the heavy-ion abundances with those measured in the fast and slow solar wind (von Steiger et al. 2000) and in particle populations accelerated near the Sun (Reames 1995a;Mason et al. 2004) and in IP space (Desai et al. 2003).”
• Up to 1‐hour forecasting of radiation hazards from solar energetic ion events with relativistic electrons (2007, background): “[124] Although the GOES >10 pfu list is characterized as mainly containing ‘‘gradual’’ events, up to three ‘‘impulsive’’ events identified in Table 1a (events 5, 49, and 61) have contributed [see, e.g., Mason et al., 2004; Kahler, 2005].”
• Shock Geometry, Seed Populations, and the Origin of Variable Elemental Composition at High Energies in Large Gradual Solar Particle Events (2005, background): “…are elevated Fe/C (and Fe/O) 10 times the average coronal and solar-wind values, large enhancements in trans-Fe ions (Reames 2000; Reames & Ng 2004; Mason et al. 2004), Fe ions with QFeh i > 16 (Luhn et al. 1987), and 3He/4He 8 CME parameters were provided by http://cdaw.gsfc.nasa.gov/CME_list.”
• The Two Sources of Solar Energetic Particles (2012, background): “In recent years it has become possible to extend abundance measurements up to the vicinity of the element Pb at Z=82 (Reames 2000; Mason et al. 2004; Reames and Ng 2004), although not with individual-element resolution above Z~30.”