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.
doi:10.1029/2010JA015615.
https://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 |
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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.
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Group: | Space Radiation Laboratory |
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Funders: | Funding Agency | Grant Number |
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NASA | NNX06AC21G | NASA | NNG04GF83G | NASA | NNG05GH38G | NASA | NNG05GM62G | NASA | NNX07AN45G | NSF | ATM0317509 | NSF | ATM0428880 |
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Subject Keywords: | SEP events; modeling; heliosphere
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Other Numbering System: | Other Numbering System Name | Other Numbering System ID |
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Space Radiation Laboratory | 2011-06 |
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DOI: | 10.1029/2010JA015615 |
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Record Number: | CaltechAUTHORS:20110119-084228407 |
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Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20110119-084228407 |
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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 |
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Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. |
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ID Code: | 21803 |
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Collection: | CaltechAUTHORS |
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Deposited By: |
Tony Diaz
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Deposited On: | 26 Jan 2011 22:22 |
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Last Modified: | 09 Nov 2021 16:00 |
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