A theoretical perspective on particle acceleration by interplanetary shocks and the Solar Energetic Particle problem

2015 ◽  
Vol 557 ◽  
pp. 1-23 ◽  
Author(s):  
Olga P. Verkhoglyadova ◽  
Gary P. Zank ◽  
Gang Li
Keyword(s):  
Particle Acceleration ◽  
Energetic Particle ◽  
Theoretical Perspective ◽  
Solar Energetic Particle ◽  
Interplanetary Shocks

scholarly journals Particle acceleration and sources in the November 1997 solar energetic particle events

1999 ◽  
Vol 26 (2) ◽  
pp. 141-144 ◽  
Author(s):  
G. M. Mason ◽  
C. M. S. Cohen ◽  
A. C. Cummings ◽  
J. R. Dwyer ◽  
R. E. Gold ◽  
...  
Keyword(s):  
Particle Acceleration ◽  
Energetic Particle ◽  
Solar Energetic Particle ◽  
Solar Energetic Particle Events

scholarly journals Fluxes and fluences of SEP events derived from SOLPENCO

2005 ◽  
Vol 23 (9) ◽  
pp. 3047-3053 ◽  
Author(s):  
A. Aran ◽  
B. Sanahuja ◽  
D. Lario
Keyword(s):  
Energetic Particle ◽  
Radial Distance ◽  
Solar Energetic Particle ◽  
Particle Energy ◽  
Particle Accelerator ◽  
Large Set ◽  
The Sun ◽  
Particle Engineering ◽  
Interplanetary Shocks ◽  
Peak Flux

Abstract. We have developed aran04 a tool for rapid predictions of proton flux and fluence profiles observed during gradual solar energetic particle (SEP) events and upstream of the associated traveling interplanetary shocks. This code, named SOLPENCO (for SOLar Particle ENgineering COde), contains a data base with a large set of interplanetary scenarios under which SEP events develop. These scenarios are basically defined by the solar longitude of the parent solar activity, ranging from E75 to W90, and by the position of the observer, located at 0.4 AU or at 1.0 AU, from the Sun. We are now analyzing the performance and reliability of SOLPENCO. We address here two features of SEP events especially relevant to space weather purposes: the peak flux and the fluence. We analyze how the peak flux and the fluence of the synthetic profiles generated by SOLPENCO vary as a function of the strength of the CME-driven shock, the heliolongitude of the solar parent activity and the particle energy considered. In particular, we comment on the dependence of the fluence on the radial distance of the observer (which does not follow an inverse square law), and we draw conclusions about the influence of the shock as a particle accelerator in terms of its evolving strength and the heliolongitude of the solar site where the SEP event originated.

scholarly journals From the Sun’s south to the north pole – Ulysses COSPIN/LET composition measurements at solar maximum

2003 ◽  
Vol 21 (6) ◽  
pp. 1383-1391 ◽  
Author(s):  
M. Y. Hofer ◽  
R. G. Marsden ◽  
T. R. Sanderson ◽  
C. Tranquille
Keyword(s):  
Energetic Particle ◽  
Solar Physics ◽  
Solar Energetic Particle ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Elemental Abundance ◽  
Interplanetary Shocks ◽  
Activity Maximum ◽  
Interplanetary Physics ◽  
Inner Heliosphere

Abstract. Based on elemental abundance ratios derived from the Ulysses COSPIN/LET measurements, we classified the energetic particle populations during and after the socalled Fast Latitude Scan – the time period during which the Ulysses spacecraft traveled from the highest heliolatitude south to maximum northern latitude, i.e. 27 November 2000 to 13 October 2001 – as being mixed between solar energetic particles (major component) and particles accelerated at stream interaction regions. During the fast latitude scan, the Ulysses spacecraft made the first transit in heliolatitude from pole to pole during solar activity maximum conditions, providing a unique opportunity to acquire energetic particle composition data over a maximum range of heliolatitudes in the inner heliosphere. At low latitudes, based on our elemental abundance analysis, we found that while solar energetic particles dominated, there were indications for particle acceleration at single compression regions in a few instances. In the high heliolatitude range the observed elemental particle compositions are mainly of the solar energetic particle type. Within the statistical errors, the observed abundance ratios were independent of latitude, and were characteristic of solar energetic particles. These observations raise an important question for the theories of particle propagation in the inner heliosphere. The daily elemental abundance ratios of S/O, Mg/O and Si/O shown here are the first measured ratios at high heliolatitudes in the energy range from 13.0 to 30.0 MeV/n.Key words. Interplanetary physics (energetic particles; interplanetary shocks) – Solar physics, astrophysics and astronomy (flares and mass ejections)

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