Abstract: Validation of Coronal and Heliospheric Models for Quasi-Steady Solar Wind: WSA-Enlil, MAS-Enlil, SWMF, and IPS Tomography Models (2014 AGU Fall Meeting)

Validation of Coronal and Heliospheric Models for Quasi-Steady Solar Wind: WSA-Enlil, MAS-Enlil, SWMF, and IPS Tomography Models

Lan Jian^1,2, Peter J MacNeice³, Aleksandre Taktakishvili^4,5, Rebekah M Evans^1,6, Dusan Odstrcil^1,7, Charles Nickolos Arge¹, Bernard V Jackson⁸, Hsiu-Shan Yu⁹, Pete Riley¹⁰ and Igor Sokolov¹¹, (1)NASA Goddard Space Flight Center, Greenbelt, MD, United States, (2)University of Maryland, College Park, College Park, MD, United States, (3)NASA Goddard Space Flight Center, Community Coordinated Modeling Center, Greenbelt, United States, (4)Catholic University of America, Washington, United States, (5)NASA Goddard Space Flight Center, Community Coordinated Modeling Center, Greenbelt, MD, United States, (6)George Mason University Fairfax, Fairfax, VA, United States, (7)George Mason University Fairfax, Physics and Astronomy, Fairfax, VA, United States, (8)University of California San Diego, Astronomy and Astrophysics, La Jolla, CA, United States, (9)Univ California San Diego, La Jolla, CA, United States, (10)Predictive Science Inc., San Diego, CA, United States, (11)University of Michigan, Climate and Space Sciences and Engineering, Ann Arbor, United States

Abstract:

Multiple coronal and heliospheric models have been recently upgraded at the Community Coordinated Modeling Center (CCMC), including the Wang-Sheely-Arge (WSA)-Enlil, MHD-around-a-sphere (MAS)-Enlil, space weather modeling framework (SWMF), and interplanetary scintillation (IPS) tomography models. We run these models for Carrington rotations 2056 – 2062 (April – November 2007), in which the solar wind was in the late declining phase and Ulysses had a fast latitudinal scan at 1.4 – 1.8 AU. We compare the modeling results with the in situ observations: OMNI data for L1, MESSENGER, Venus Express and Ulysses, all together covering 0.3 – 1.8 AU. We assess the capabilities of these models in capturing quasi-steady solar wind features including sector boundaries and the fast-slow stream interaction regions. For this particular period, we derive the strengths, weaknesses, and discrepancies from observations for each model, and discuss the effect of photospheric magnetograms from different observatories, such as GONG and SOLIS magnetograms from National Solar Observatory (NSO) and magnetograms from Mount Wilson Observatory (MWO).

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