4.2 Article

Corotating interaction regions during the recent solar minimum: The power and limitations of global MHD modeling

Journal

Publisher

PERGAMON-ELSEVIER SCIENCE LTD
DOI: 10.1016/j.jastp.2011.12.013

Keywords

Corona; Solar wind; Corotating interaction regions; Magnetohydrodynamics; Space weather

Funding

  1. NSF under the Center for Integrated Space Weather Modeling (CISM) program
  2. LWS Strategic Capabilities Program (NASA, NSF, and AFOSR)
  3. NASA's Heliophysics Theory Program (HTP)
  4. STEREO IMPACT team
  5. NASA's Causes and Consequences of the Minimum of Solar Cycle 24 program
  6. Universidad Nacional Autonoma de Mexico (UNAM)
  7. Directorate For Geosciences
  8. Div Atmospheric & Geospace Sciences [1138256] Funding Source: National Science Foundation

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The declining phase of solar activity cycle 23 has provided an unprecedented opportunity to study the evolution and properties of corotating interaction regions (CIRs) during unique and relatively steady conditions. The absence of significant transient activity has allowed modelers to test ambient solar wind models, but has also challenged them to reproduce structure that was qualitatively different than had been observed previously (at least within the space era). In this study, we present and analyze global magnetohydrodynamic (MHD) solutions of the inner heliosphere (from 1R(S) to 1 AU) for several intervals defined as part of a Center for Integrated Space weather Modeling (CISM) interdisciplinary campaign study, and, in particular, Carrington rotation 2060. We compare in situ measurements from ACE and STEREO A and B with the model results to illustrate both the capabilities and limitations of current numerical techniques. We show that, overall, the models do capture the essential structural features of the solar wind for specific time periods; however, there are times when the models and observations diverge. We describe, and, to some extent assess the sources of error in the modeling chain from the input photospheric magnetograms to the numerical schemes used to propagate structure through the heliosphere, and speculate on how they may be resolved, or at least mitigated in the future. (C) 2011 Elsevier Ltd. All rights reserved.

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