Synthesis of 3-D coronal-solar wind energetic particle acceleration modules

Authors

Nathan A. Schwadron, University of New HampshireFollow
Matthew J. Gorby, University of New HampshireFollow
Tibor Torak, Predictive Science Inc
Cooper Downs, Predictive Science Inc
J. A. Linker, Predictive Science Inc.Follow
Roberto Lionello, Predictive Science Inc
Z. Mikic, Predictive Science Inc.Follow
P. Riley, Predictive Science Inc.Follow
Joe Giacalone, University of Arizona
Benjamin D.G. Chandran, University of New HampshireFollow
Kai K. Germaschewski, University of New HampshireFollow
Philip A. Isenberg, University of New HampshireFollow
Martin A. Lee, University of New Hampshire - Main CampusFollow
Noe E. Lugaz, University of New Hampshire - Main CampusFollow
Sonya S. Smith, University of New HampshireFollow
Harlan E. Spence, University of New HampshireFollow
M. Desai, Southwest Research InstituteFollow
J. C. Kasper, University of New HampshireFollow
K. Kozarev, University of Michigan - Ann ArborFollow
K. E. Korreck, University of Michigan - Ann ArborFollow
M. L. Stevens, University of Michigan - Ann ArborFollow
J. F. Cooper, Smithsonian Astrophysical ObservatoryFollow
Peter MacNeice, Goddard Space Flight Center.

Abstract

1. Introduction Acute space radiation hazards pose one of the most serious risks to future human and robotic exploration. Large solar energetic particle (SEP) events are dangerous to astronauts and equipment. The ability to predict when and where large SEPs will occur is necessary in order to mitigate their hazards. The Coronal-Solar Wind Energetic Particle Acceleration (C-SWEPA) modeling effort in the NASA/NSF Space Weather Modeling Collaborative [Schunk, 2014] combines two successful Living With a Star (LWS) (http://lws. gsfc.nasa.gov/) strategic capabilities: the Earth-Moon-Mars Radiation Environment Modules (EMMREM) [Schwadron et al., 2010] that describe energetic particles and their effects, with the Next Generation Model for the Corona and Solar Wind developed by the Predictive Science, Inc. (PSI) group. The goal of the C-SWEPA effort is to develop a coupled model that describes the conditions of the corona, solar wind, coronal mass ejections (CMEs) and associated shocks, particle acceleration, and propagation via physics-based modules. Assessing the threat of SEPs is a difficult problem. The largest SEPs typically arise in conjunction with X class flares and very fast (>1000 km/s) CMEs. These events are usually associated with complex sunspot groups (also known as active regions) that harbor strong, stressed magnetic fields. Highly energetic protons generated in these events travel near the speed of light and can arrive at Earth minutes after the eruptive event. The generation of these particles is, in turn, believed to be primarily associated with the shock wave formed very low in the corona by the passage of the CME (injection of particles from the flare site may also play a role). Whether these particles actually reach Earth (or any other point) depends on their transport in the interplanetary magnetic field and their magnetic connection to the shock.

Department

Physics

Publication Date

6-2014

Journal Title

Space Weather

Publisher

American Geophysical Union Publications

Digital Object Identifier (DOI)

10.1002/2014SW001086

Document Type

Article

Recommended Citation

Schwadron, N.A., Gorby, M., Török, T., Downs, C., Linker, J., Lionello, R., Mikic̈, Z., Riley, P., Giacalone, J., Chandran, B., Germaschewski, K., Isenberg, P.A., Lee, M.A., Lugaz, N., Smith, S., Spence, H.E., Desai, M., Kasper, J., Kozarev, K., Korreck, K., Stevens, M., Cooper, J., Macneice, P. Synthesis of 3-D coronal-solar wind energetic particle acceleration modules. (2014) Space Weather, 12 (6), pp. 323-328. doi:10.1002/2014SW001086

Rights

©2014. American Geophysical Union. All Rights Reserved.