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3D Reconstruction of Interplanetary Scintillation (IPS) Remote-Sensing Data: Global Solar Wind Boundaries for Driving 3D-MHD Models

  • Radio Heliophysics: Science and Forecasting
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Abstract

The University of California, San Diego, time-dependent analyses of the heliosphere provide three-dimensional (3D) reconstructions of solar wind velocities and densities from observations of interplanetary scintillation (IPS). Using data from the Solar-Terrestrial Environment Laboratory, Japan, these reconstructions provide a real-time prediction of the global solar-wind density and velocity throughout the whole heliosphere with a temporal cadence of about one day ( ips.ucsd.edu ). Updates to this modeling effort continue: in the present article, near-Sun results extracted from the time-dependent 3D reconstruction are used as inner boundary conditions to drive 3D-MHD models (e.g. ENLIL and H3D-MHD). This allows us to explore the differences between the IPS kinematic-model data-fitting procedure and current 3D-MHD modeling techniques. The differences in these techniques provide interesting insights into the physical principles governing the expulsion of coronal mass ejections (CMEs). Here we detail for the first time several specific CMEs and an induced shock that occurred in September 2011 that demonstrate some of the issues resulting from these analyses.

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Acknowledgements

H.-S. Yu, B.V. Jackson, P.P. Hick, and A. Buffington were supported at UCSD by NSF grants AGS-1053766, and AGS-1358399, and by AFOSR grant FA9550-11-1-0324. Work of C.-C. Wu was supported by the ONR 6.1 program. The authors wish to acknowledge and thank the group at STELab, Nagoya University (those not included in the author list: M. Kojima, K. Fujiki, and students) for their continued support, and for making IPS data sets available under the auspices of a joint collaborative agreement between the Center for Astrophysics and Space Sciences at UCSD and STELab, Nagoya University. We wish to thank Kevin Schenk and the LASCO coronagraph group for the CME images taken using the C2 coronagraph, and the STEREO/SECCHI group for making available their COR2 images. We also thank the UKSSDC (UK solar system data centre) for providing the HI data.

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Authors and Affiliations

  1. Center for Astrophysics and Space Sciences, University of California at San Diego, 9500 Gilman Drive #0424, La Jolla, CA, 92093-0424, USA

    H.-S. Yu, B. V. Jackson, P. P. Hick & A. Buffington

  2. George Mason University, 4400 University Drive, Fairfax, VA, 22030, USA

    D. Odstrcil

  3. NASA/GSFC M/C 674, Greenbelt, MD, 20771, USA

    D. Odstrcil

  4. Naval Research Laboratory, 4555 Overlook Ave., Washington, DC, 20375, USA

    C.-C. Wu

  5. RAL Space, Science & Technology Facilities Council – Rutherford Appleton Laboratory, Harwell Oxford, Didcot, OX11 0QX, UK

    J. A. Davies & M. M. Bisi

  6. Solar-Terrestrial Environment Laboratory (STELab), Nagoya University, Furo-cho, Chikusa-ku, Nagoya, 464-8601, Japan

    M. Tokumaru

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  1. H.-S. Yu
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Radio Heliophysics: Science and Forecasting

Guest Editors: Mario M. Bisi, Bernard V. Jackson, and J. Americo Gonzalez-Esparza

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Yu, HS., Jackson, B.V., Hick, P.P. et al. 3D Reconstruction of Interplanetary Scintillation (IPS) Remote-Sensing Data: Global Solar Wind Boundaries for Driving 3D-MHD Models. Sol Phys 290, 2519–2538 (2015). https://doi.org/10.1007/s11207-015-0685-0

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