HIIS results on the mean ionic charge state of SEP Fe above 200 MeV per nucleon

Tylka, A. J.; Boberg, P. R.; Adams, J. H.; Beahm, Lorraine P.; Dietrich, William F.; Kleis, T.

doi:10.1063/1.50992

Cited by 3 publications

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“…Kahler's result is consistent with the idea that the solar energetic particles observed in interplanetary space after gradual flares are accelerated in shocks driven by the CMEs. Above 100 MeV/nucleon the charge state measurements by Tylka et al (1996) also indicate that the interplanetary particles are characteristic of the solar corona. In addition, expanded Reames' tabular summary of the two-class picture of interplanetary solar particle events and argued that gradual solar flare events "can be expected to have a temporally and spatially confined core of flare-accelerated particles surrounded by a halo of CME/shock particles".…”

Section: Expected Angle Distribution and Time Variations Of Gamma Raymentioning

confidence: 93%

Solar Neutrons and Related Phenomena

Дорман¹

2010

Astrophysics and Space Science Library

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Section: Expected Angle Distribution and Time Variations Of Gamma Raymentioning

confidence: 93%

Solar Neutrons and Related Phenomena

Дорман¹

2010

Astrophysics and Space Science Library

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“…This time corresponded to the arrival near Earth of a powerful interplanetary shock, driven by the fast coronal mass ejection which erupted from near the center of the solar disk on the previous day. This period contained the highest particle fluxes of the entire week-long disturbance, with the shock raising fluxes by roughly another order of magnitude for -3-6 hours [36], [41].…”

Section: Solar Particle ("Flare") Eventsmentioning

confidence: 99%

CREME96: A Revision of the Cosmic Ray Effects on Micro-Electronics Code

Tylka

Adams

Boberg³

et al. 1997

IEEE Trans. Nucl. Sci.

551

254

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A bstTactCREME96 is an update of the Cosmic Ray Effects on Micro-Electronics code, a widely-used suite of programs for creating numerical models of the ionizingradiation environment in near-Earth orbits and for evaluating radiation effects in spacecraft. CREME96, which is now available over the World-Wide Web (WWW) at http://crsp3.nrl.navy.mil/creme96/, has many significant features, including (1) improved models of the galactic cosmic ray, anomalous cosmic ray, and solar energetic particle ("flare") components of the near-Earth environment;(2) improved geomagnetic transmission calculations; (3) improved nuclear transport routines; (4) improved singleevent upset (SEU) calculation techniques, for both protoninduced and direct-ionization-induced SEUs; and (5) an easy-to-use graphical interface, with extensive on-line tutorial information. In this paper we document some of these improvements. b ! ~ I I

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“…Difficulties in transporting SEPs across magnetic field lines over 180°in solar longitude were surmounted by the mathematically contrived "coronal diffusion," which had scant basis in physics. The demise of the flare myth began when SEP ionization states were measured that were much too low for the temperatures in a solar flare (12,24). At about the same time, the relationship between CMEs, shocks, and SEPs began to emerge…”

Section: Introductionmentioning

confidence: 99%

The observational consequences of proton-generated waves at shocks

Reames

2000

AIP Conference Proceedings

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Abstract. In the largest solar energetic particle (SEP) events, acceleration takes place at shock waves driven out from the Sun by fast coronal mass ejections. Protons streaming away from strong shocks generate Alfv_n waves that trap particles in the acceleration region, limiting outflowing intensities but increasing the efficiency of acceleration to higher energies. Early in the events, with the shock still near the Sun, intensities at 1 AU are bounded and spectra are flattened at low energies. Elements with different charge-to-mass ratios, Q/A, differentially probe the wave spectra near shocks, producing abundance ratios that vary in space and time. An initial rise in He/H, while Felt declines, is a typical symptom of the non-Kolmogorov wave spectra in the largest events. Strong wave generation can cause cross-field scattering near the shock and unusually rapid reduction in anisotropies even far from the shock. At the highest energies, shock spectra steepen to form a "knee." For protons, this spectral knee can vary from -10 MeV to -1 GeV depending on shock conditions for wave growth. In one case, the location of the knee scales approximately as Q/A in the energy/nucleon spectra of other species.

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HIIS results on the mean ionic charge state of SEP Fe above 200 MeV per nucleon

Cited by 3 publications

References 0 publications

Solar Neutrons and Related Phenomena

Solar Neutrons and Related Phenomena

CREME96: A Revision of the Cosmic Ray Effects on Micro-Electronics Code

The observational consequences of proton-generated waves at shocks

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