1 Center for Astrophysics and Space Sciences, University of California, San Diego 9500 Gilman Drive #0424, La Jolla, CA , U.S.A 2 Center for Space Plasma and Aeronomic Research, The University of Alabama in Huntsville, Huntsville, AL, U.S.A. 3 Naval Research Laboratory, Washington, DC, U.S.A. THE 3D RECONSTRUCTED GLOBAL SOLAR WIND BOUNDARY FROM REMOTE-SENSING IPS DATA Hsiu-Shan Yu 1, B.V. Jackson 1, P.P. Hick 1, A. Buffington 1, Tae K. Kim 2 Nikolai V. Pogorelov 2, and Chin-Chun Wu 3 Hsiu-Shan Yu 1, B.V. Jackson 1, P.P. Hick 1, A. Buffington 1, Tae K. Kim 2, Nikolai V. Pogorelov 2, and Chin-Chun Wu 3Abstract The University of California, San Diego (UCSD) interplanetary scintillation (IPS) remote-sensing analyses of the heliosphere have measured and reconstructed 3D solar wind velocities and densities for nearly two decades. These global results, especially using Solar-Terrestrial Environment Laboratory (STELab) IPS observations, provide time- dependent density and velocity that is nearly complete over the whole heliosphere for the major part of each year and with a time cadence of about one day. The IPS volumetric velocity from this time-dependent tomography accurately convects solar surface magnetic fields outward and thus provides values of the magnetic field throughout the global volume. Therefore, we can extract these parameters at any height in the inner heliosphere and use it as an inner "boundary" for MHD models. Here we present sample determinations of the global solar wind boundaries we have provided for 3D-MHD models from recent IPS data sets. Preliminary 3D-MHD modeling results from two different modelling efforts are shown using these boundaries. 2. IPS Time-Dependent 3D Tomographic Reconstructions Global Remote View Density Meridional Cut Density Ecliptic Cut Density Enhancement at the East of Sun-Earth Line Slight Density Increase at Earth 1. Interplanetary Scintillation (IPS) Solar-Terrestrial Environment Laboratory (STELab) radio array, Japan; the Fuji system is shown. USCD currently maintains a near-real-time website that analyzes and displays IPS data from the STELab. This modeling- analysis capability is also available at the CCMC. STELab Website: USCD Real-Time Website: CCMC Website: USCD Real-Time Website: http//:ips.ucsd.edu/ CCMC Website: App/index.jsp? Interplanetary Scintillation (IPS) observations have long been used to remotely-sense small-scale ( km) heliospheric density variation along the line of sight in the solar wind. These density inhomogeneities in the solar wind disturb the signal from point radio sources to produce an intensity variation projected on the ground whose pattern travels away from the Sun with the solar wind speed. This pattern, measured and correlated between different radio sites in Japan allows a determination of the solar wind speed. By cross-correlating the radio signal obtained at different IPS observing sites, we determine the solar wind speed. By measuring the scintillation strength of the IPS source, we can also determine the solar wind density. STELab IPS array systems 500 km [Jackson et al., Solar Phys., 2010; and Jackson, et al., Solar Phys, 2012 (in press)] IPS Fish-Eye Map 2011 November 09 Halo CME LASCO C2 STEREO COR-2B A slightly earlier CME moves outward to the southeast and is more towards the Earth. The same disturbance is seen by both STEREO-COR2B A dominant CME in the LASCO C2 field of view travels rapidly to the solar northeast and is more distant from the Earth.

3. Global Solar Wind Boundary Time-Dependent Boundary in Inertial Heliographic Coordinates (IHG) (Upper panels) Density (a), velocity (b), and radial (c) and tangential (d) magnetic field inner boundaries for MS-FLUKSS 3-D MHD modeling (Tae et. al, 2012) extracted at 0.25AU from 3D time-dependent tomography using STELab IPS observations and NSO magnetograms. (Right panels) Comparisons of the 3-D MHD simulation results using time-dependent IPS boundaries with the OMNI data and UCSD kinematic solutions. 4. Summary and Discussion The analysis of IPS data provides low-resolution global measurements of density and velocity with a time cadence of one day for both density and velocity, and slightly longer cadences for some magnetic field components. Accurate observations of inner heliosphere parameters coupled with the best physics can extrapolate these outward to Earth or the interstellar boundary. For current specific applications it is best to certify that there are high-quality data (both remotely-sensed and in situ) available for the periods of study, especially when using these analyses as a lower boundary for 3D-MHD forward-modeling techniques. The 3-D MHD simulation results using IPS boundaries as input compare fairly well with in situ measurements. References Jackson, B.V., Hick, P.P., Bisi, M.M., Clover, J.M., and Buffington, A., 2012, “Inclusion of Real-Time in-situ Measurements into the UCSD Time-Dependent Tomography and Its Use as a Forecast Algorithm”, Solar Phys., (in press). Jackson, B.V., Hick, P.P., Buffington, A., Clover, J.M., and Tokumaru, M., 2012, “Forecasting Transient Heliospheric Solar Wind Parameters at the Locations of the Inner Planets”, Adv. in Geosciences, 30, Kim, T. K., N.V. Pogorelov, S.N. Borovikov, J.M. Clover, B.V. Jackson, H.-S. Yu, G. Li, G.P. Zank, X. Ao, O. Verkhoglyadova, J.H. Adams, 2012, “Time-dependent MHD simulations of the solar wind outflow using interplanetary scintillation observations”, AIP Conference 1500, pp Wu, S. T., H. Zheng, S. Wang, B.J. Thompson, S.P. Plunkett, X.P. Zhao, M. Dryer, 2001, “Three-dimensional numerical simulation of MHD waves observed by the Extreme Ultraviolet Imaging Telescope”, J. Geophys. Res. 106, Time-Dependent Boundary in Heliographic Coordinates (Earth-Centered)  marks the Earth subsolar point. (Upper panels) Density (a), and velocity (b) inner boundaries for 3-D MHD modeling (Wu et. al, 2001). (Lower panels) Comparison of the 3-D MHD results with WIND data.