TY - JOUR
T1 - SPECTRAL PROPERTIES of LARGE GRADUAL SOLAR ENERGETIC PARTICLE EVENTS. II. SYSTEMATIC Q/M DEPENDENCE of HEAVY ION SPECTRAL BREAKS
AU - Desai, M. I.
AU - Mason, G. M.
AU - Dayeh, M. A.
AU - Ebert, R. W.
AU - McComas, D. J.
AU - Li, G.
AU - Cohen, C. M.S.
AU - Mewaldt, R. A.
AU - Schwadron, N. A.
AU - Smith, C. W.
N1 - Funding Information:
We acknowledge use of the NOAA GOES and SOHO/ERNE proton data. Work at SwRI is partially supported by NASA grants NNX13AE07G and NNX13AI75G, NASA contracts NNX10AT75G and NNN06AA01C, and NSF Grants AGS-1135432 and AGS- 1460118. Work at APL was supported by NASA grants NNX13AR20G/115828 and 44A-1091698.
Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.
PY - 2016/9/10
Y1 - 2016/9/10
N2 - We fit ∼0.1-500 MeV nucleon-1 H-Fe spectra in 46 large solar energetic particle (SEP) events with the double power-law Band function to obtain a normalization constant, low- and high-energy parameters γ a and γ b, and break energy E B, and derive the low-energy spectral slope γ 1. We find that: (1) γ a, γ 1, and γ b are species-independent and the spectra steepen with increasing energy; (2) E B decreases systematically with decreasing Q/M scaling as (Q/M)α; (3) α varies between ∼0.2-3 and is well correlated with the ∼0.16-0.23 MeV nucleon-1 Fe/O; (4) in most events, α < 1.4, γ b-γ a > 3, and O E B increases with γ b-γ a; and (5) in many extreme events (associated with faster coronal mass ejections (CMEs) and GLEs), Fe/O and 3He/4He ratios are enriched, α ≥ 1.4, γ b-γ a < 3, and E B decreases with γ b-γ a. The species-independence of γ a, γ 1, and γ b and the Q/M dependence of E B within an event and the α values suggest that double power-law SEP spectra occur due to diffusive acceleration by near-Sun CME shocks rather than scattering in interplanetary turbulence. Using γ 1, we infer that the average compression ratio for 33 near-Sun CME shocks is 2.49 0.08. In most events, the Q/M dependence of E B is consistent with the equal diffusion coefficient condition and the variability in α is driven by differences in the near-shock wave intensity spectra, which are flatter than the Kolmogorov turbulence spectrum but weaker than the spectra for extreme events. In contrast, in extreme events, enhanced wave power enables faster CME shocks to accelerate impulsive suprathermal ions more efficiently than ambient coronal ions.
AB - We fit ∼0.1-500 MeV nucleon-1 H-Fe spectra in 46 large solar energetic particle (SEP) events with the double power-law Band function to obtain a normalization constant, low- and high-energy parameters γ a and γ b, and break energy E B, and derive the low-energy spectral slope γ 1. We find that: (1) γ a, γ 1, and γ b are species-independent and the spectra steepen with increasing energy; (2) E B decreases systematically with decreasing Q/M scaling as (Q/M)α; (3) α varies between ∼0.2-3 and is well correlated with the ∼0.16-0.23 MeV nucleon-1 Fe/O; (4) in most events, α < 1.4, γ b-γ a > 3, and O E B increases with γ b-γ a; and (5) in many extreme events (associated with faster coronal mass ejections (CMEs) and GLEs), Fe/O and 3He/4He ratios are enriched, α ≥ 1.4, γ b-γ a < 3, and E B decreases with γ b-γ a. The species-independence of γ a, γ 1, and γ b and the Q/M dependence of E B within an event and the α values suggest that double power-law SEP spectra occur due to diffusive acceleration by near-Sun CME shocks rather than scattering in interplanetary turbulence. Using γ 1, we infer that the average compression ratio for 33 near-Sun CME shocks is 2.49 0.08. In most events, the Q/M dependence of E B is consistent with the equal diffusion coefficient condition and the variability in α is driven by differences in the near-shock wave intensity spectra, which are flatter than the Kolmogorov turbulence spectrum but weaker than the spectra for extreme events. In contrast, in extreme events, enhanced wave power enables faster CME shocks to accelerate impulsive suprathermal ions more efficiently than ambient coronal ions.
KW - Sun: abundances
KW - Sun: flares
KW - acceleration of particles
KW - interplanetary medium
KW - shock waves
KW - solar wind
UR - http://www.scopus.com/inward/record.url?scp=84991608430&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84991608430&partnerID=8YFLogxK
U2 - 10.3847/0004-637X/828/2/106
DO - 10.3847/0004-637X/828/2/106
M3 - Article
AN - SCOPUS:84991608430
VL - 828
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 106
ER -