scholarly journals Empirical Model of 10 – 130 MeV Solar Energetic Particle Spectra at 1 AU Based on Coronal Mass Ejection Speed and Direction

Solar Physics ◽  
2021 ◽  
Vol 296 (2) ◽  
Author(s):  
Alessandro Bruno ◽  
Ian G. Richardson
Keyword(s):  
Coronal Mass Ejection ◽  
Empirical Model ◽  
Energetic Particle ◽  
Solar Energetic Particle ◽  
Particle Spectra ◽  
Ejection Speed ◽  
Mass Ejection

scholarly journals Strength of Coronal Mass Ejection‐driven Shocks near the Sun and Their Importance in Predicting Solar Energetic Particle Events

2007 ◽  
Vol 670 (1) ◽  
pp. 849-856 ◽  
Author(s):  
Chenglong Shen ◽  
Yuming Wang ◽  
Pinzhong Ye ◽  
X. P. Zhao ◽  
Bin Gui ◽  
...  
Keyword(s):  
Coronal Mass Ejection ◽  
Energetic Particle ◽  
Solar Energetic Particle ◽  
The Sun ◽  
Solar Energetic Particle Events ◽  
Mass Ejection

scholarly journals Nowcasting of Solar Energetic Particle Events using near real-time Coronal Mass Ejection characteristics in the framework of the FORSPEF tool

2018 ◽  
Vol 8 ◽  
pp. A37 ◽  
Author(s):  
Athanasios Papaioannou ◽  
Anastasios Anastasiadis ◽  
Ingmar Sandberg ◽  
Piers Jiggens
Keyword(s):  
Coronal Mass Ejection ◽  
Real Time ◽  
Energetic Particle ◽  
Solar Energetic Particle ◽  
Probability Of Detection ◽  
Angular Width ◽  
Link Type ◽  
Halo Cmes ◽  
Mass Ejection ◽  
Archived Data

In this work the derived occurrence probability of solar energetic particle (SEP) events (i.e. proton events measured at Earth’s position) and their peak fluxes and total fluences depending on coronal mass ejection (CME) parameters, i.e. linear speed (V) and the angular width (AW) are presented. A new SEP catalogue with associated CME data from 1997 to 2013 is utilized. It is found that the SEP probability strongly depends on the CME speed and the angular width as follows: The highest association (72.70%) is obtained for the full halo CMEs with V ≥ 1500 km s−1 and the lowest association (0.7%) is found for the non halo CMEs with 400 km s−1 ≤ V ≤ 1000 km s−1. The SEP occurrence probabilities are different as much as 26 times according to the CME speed (V), comparing fast versus slow CMEs and 44 times according to the AW, comparing halo to non halo CMEs. Furthermore, linear regressions of the proton peak flux and integral fluence at several integral energy channels (E > 10 MeV, E > 30 MeV, E > 60 MeV, E > 100 MeV) were obtained. Our results, were used to build a module of an operational forecasting tool (i.e. FORecasting Solar Particle Events and Flares – FORSPEF, http://tromos.space.noa.gr/forspef/). This module performs nowcasting (short term forecasting) of SEP events using near real-time CME identifications obtained from CACTus (http://sidc.oma.be/cactus/). The outputs offered by the operational module of the tool to the end user (textural, pictorial, archived data) are presented. Finally, the validation of the system, in terms of archived data is described, in terms of categorical scores (Probability of Detection – POD and a False Alarm Rate – FAR).

scholarly journals Multipoint observations of coronal mass ejection and solar energetic particle events on Mars and Earth during November 2001

2011 ◽  
Vol 116 (A6) ◽  
pp. n/a-n/a ◽  
Author(s):  
T. V. Falkenberg ◽  
S. Vennerstrom ◽  
D. A. Brain ◽  
G. Delory ◽  
A. Taktakishvili
Keyword(s):  
Coronal Mass Ejection ◽  
Energetic Particle ◽  
Solar Energetic Particle ◽  
Solar Energetic Particle Events ◽  
Mass Ejection
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