High-energy solar particles and human exploration

Space Weather ◽  
2005 ◽  
Vol 3 (5) ◽  
pp. n/a-n/a ◽  
Author(s):  
Louis J. Lanzerotti
Keyword(s):  
High Energy ◽  
Solar Particles ◽  
Human Exploration

scholarly journals Common overabundance of $\mathsf{^3}$He in high-energy solar particles

2003 ◽  
Vol 408 (1) ◽  
pp. L1-L4 ◽  
Author(s):  
J. Torsti ◽  
J. Laivola ◽  
L. Kocharov
Keyword(s):  
High Energy ◽  
Solar Particles

Neutron monitor observations of high-energy solar particles during the new cycle

Solar Physics ◽  
1967 ◽  
Vol 2 (4) ◽  
Author(s):  
G.A. Baird ◽  
G.G. Bell ◽  
S.P. Duggal ◽  
M.A. Pomerantz
Keyword(s):  
Neutron Monitor ◽  
High Energy ◽  
Solar Particles

scholarly journals PAMELA’S MEASUREMENTS OF MAGNETOSPHERIC EFFECTS ON HIGH-ENERGY SOLAR PARTICLES

2015 ◽  
Vol 801 (1) ◽  
pp. L3 ◽  
Author(s):  
O. Adriani ◽  
G. C. Barbarino ◽  
G. A. Bazilevskaya ◽  
R. Bellotti ◽  
M. Boezio ◽  
...  
Keyword(s):  
High Energy ◽  
Solar Particles

scholarly journals GLE # 67 Event on 2 November 2003: An Analysis of the Spectral and Anisotropy Characteristics Using Verified Yield Function and Detrended Neutron Monitor Data

Solar Physics ◽  
2021 ◽  
Vol 296 (5) ◽  
Author(s):  
Alexander L. Mishev ◽  
Sergey A. Koldobskiy ◽  
Leon G. Kocharov ◽  
Ilya G. Usoskin
Keyword(s):  
Neutron Monitor ◽  
Dynamical Evolution ◽  
Ground Level ◽  
High Energy ◽  
Yield Function ◽  
Angle Distribution ◽  
Ground Level Enhancement ◽  
Solar Particles ◽  
Monitor Data

AbstractDuring Solar Cycle 23 16 ground-level enhancement events were registered by the global neutron monitor network. In this work we focus on the period with increased solar activity during late October – early November 2003 producing a sequence of three events, specifically on ground-level enhancement GLE 67 on 2 November 2003. On the basis of an analysis of neutron monitor and space-borne data we derived the spectra and pitch-angle distribution of high-energy solar particles with their dynamical evolution throughout the event. According to our analysis, the best fit of the spectral and angular properties of solar particles was obtained by a modified power-law rigidity spectrum and a double Gaussian, respectively. The derived angular distribution is consistent with the observations where an early count rate increase at Oulu neutron monitor with asymptotic viewing direction in the anti-Sun direction was registered. The quality of the fit and model constraints were assessed by a forward modeling. The event integrated particle fluence was derived using two different methods. The derived results are briefly discussed.

scholarly journals Inferred charge states of high energy solar particles from the solar isotope spectrometer on ACE

1999 ◽  
Vol 26 (2) ◽  
pp. 149-152 ◽  
Author(s):  
C. M. S. Cohen ◽  
A. C. Cummings ◽  
R. A. Leske ◽  
R. A. Mewaldt ◽  
E. C. Stone ◽  
...  
Keyword(s):  
High Energy ◽  
Solar Particles ◽  
Charge States

scholarly journals Observation of high energy solar particles on September 29, 1989 by neutron monitors with high time resolution.

1990 ◽  
Vol 66 (1) ◽  
pp. 10-14 ◽  
Author(s):  
Kazuyoshi TAKAHASHI ◽  
Masami WADA ◽  
Emiko SAKAMOTO ◽  
Masaru MATSUOKA ◽  
Kazuoki MUNAKATA ◽  
...  
Keyword(s):  
Time Resolution ◽  
High Energy ◽  
High Time ◽  
High Time Resolution ◽  
Neutron Monitors ◽  
Solar Particles

scholarly journals What is Causing the Deficit of High-Energy Solar Particles in Solar Cycle 24?

2017 ◽  
Author(s):  
Richard Mewaldt ◽  
Gang Li ◽  
Junxiang Hu ◽  
Christina Cohen
Keyword(s):  
Solar Cycle ◽  
High Energy ◽  
Solar Cycle 24 ◽  
Solar Particles ◽  
Cycle 24

The E-ring: interactions with plasma and implications for its evolution

1984 ◽  
Vol 75 ◽  
pp. 599-602
Author(s):  
T.V. Johnson ◽  
G.E. Morfill ◽  
E. Grun
Keyword(s):  
Time Scale ◽  
Particle Density ◽  
High Energy ◽  
Particle Removal ◽  
Density Region ◽  
Drag Forces ◽  
Orbit Evolution ◽  
History Of ◽  
Ring Particle ◽  
Ring Material

A number of lines of evidence suggest that the particles making up the E-ring are small, on the order of a few microns or less in size (Terrile and Tokunaga, 1980, BAAS; Pang et al., 1982 Saturn meeting; Tucson, AZ). This suggests that a variety of electromagnetic and plasma affects may be important in considering the history of such particles. We have shown (Morfill et al., 1982, J. Geophys. Res., in press) that plasma drags forces from the corotating plasma will rapidly evolve E-ring particle orbits to increasing distance from Saturn until a point is reached where radiation drag forces acting to decrease orbital radius balance this outward acceleration. This occurs at approximately Rhea's orbit, although the exact value is subject to many uncertainties. The time scale for plasma drag to move particles from Enceladus' orbit to the outer E-ring is ~104yr. A variety of effects also act to remove particles, primarily sputtering by both high energy charged particles (Cheng et al., 1982, J. Geophys. Res., in press) and corotating plasma (Morfill et al., 1982). The time scale for sputtering away one micron particles is also short, 102 - 10 yrs. Thus the detailed particle density profile in the E-ring is set by a competition between orbit evolution and particle removal. The high density region near Enceladus' orbit may result from the sputtering yeild of corotating ions being less than unity at this radius (e.g. Eviatar et al., 1982, Saturn meeting). In any case, an active source of E-ring material is required if the feature is not very ephemeral - Enceladus itself, with its geologically recent surface, appears still to be the best candidate for the ultimate source of E-ring material.

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