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Understanding large SEP events with the PATH code: Modeling of the 13 December 2006 SEP event

Verkhoglyadova, O. P. and Li, G. and Zank, G. P. and Hu, Q. and Cohen, C. M. S. and Mewaldt, R. A. and Mason, G. M. and Haggerty, D. K. and von Rosenvinge, T. T. and Looper, M. D. (2010) Understanding large SEP events with the PATH code: Modeling of the 13 December 2006 SEP event. Journal of Geophysical Research A, 115 . Art. No. A12103. ISSN 0148-0227. http://resolver.caltech.edu/CaltechAUTHORS:20110119-084228407

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Abstract

The Particle Acceleration and Transport in the Heliosphere (PATH) numerical code was developed to understand solar energetic particle (SEP) events in the near-Earth environment. We discuss simulation results for the 13 December 2006 SEP event. The PATH code includes modeling a background solar wind through which a CME-driven oblique shock propagates. The code incorporates a mixed population of both flare and shock-accelerated solar wind suprathermal particles. The shock parameters derived from ACE measurements at 1 AU and observational flare characteristics are used as input into the numerical model. We assume that the diffusive shock acceleration mechanism is responsible for particle energization. We model the subsequent transport of particles originated at the flare site and particles escaping from the shock and propagating in the equatorial plane through the interplanetary medium. We derive spectra for protons, oxygen, and iron ions, together with their time-intensity profiles at 1 AU. Our modeling results show reasonable agreement with in situ measurements by ACE, STEREO, GOES, and SAMPEX for this event. We numerically estimate the Fe/O abundance ratio and discuss the physics underlying a mixed SEP event. We point out that the flare population is as important as shock geometry changes during shock propagation for modeling time-intensity profiles and spectra at 1 AU. The combined effects of seed population and shock geometry will be examined in the framework of an extended PATH code in future modeling efforts.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1029/2010JA015615 DOIArticle
ORCID:
AuthorORCID
Cohen, C. M. S.0000-0002-0978-8127
Mason, G. M.0000-0003-2169-9618
Additional Information:© 2010 American Geophysical Union. Received 28 April 2010; accepted 7 October 2010; published 7 December 2010. This work is supported in part by NASA grants NNX06AC21G, NNG04GF83G, NNG05GH38G, NNG05GM62G, and NNX07AN45G (for the EPAM and ULEIS work at APL) and NSF grants ATM0317509 and ATM0428880. Philippa Browning thanks Mathew Owens and two other reviewers for their assistance in evaluating this paper.
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASANNX06AC21G
NASANNG04GF83G
NASANNG05GH38G
NASANNG05GM62G
NASANNX07AN45G
NSFATM0317509
NSFATM0428880
Subject Keywords:SEP events; modeling; heliosphere
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2011-06
Record Number:CaltechAUTHORS:20110119-084228407
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20110119-084228407
Official Citation:Verkhoglyadova, O. P., G. Li, G. P. Zank, Q. Hu, C. M. S. Cohen, R. A. Mewaldt, G. M. Mason, D. K. Haggerty, T. T. von Rosenvinge, and M. D. Looper (2010), Understanding large SEP events with the PATH code: Modeling of the 13 December 2006 SEP event, J. Geophys. Res., 115, A12103, doi:10.1029/2010JA015615
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21803
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:26 Jan 2011 22:22
Last Modified:11 Sep 2017 17:32

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