B.V. Jackson, and P.P. Hick, A. Buffington, J.M. Clover,

1. 3-D Reconstruction of the Inner Heliosphere: A Global Solar Wind Boundary From Remote-Sensing Data B.V. Jackson, and P.P. Hick, A. Buffington, J.M. Clover, Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA and D.B. Reisenfeld, T.R. Abell Department of Physics and Astronomy, University of Montana, Missoula, MT, USA Masayoshi http://smei.ucsd.edu/ http://ips.ucsd.edu/

2. Introduction: The Motive: 3-D Interstellar boundary The Analysis: 3-D Heliospheric Tomography – (a fit to data) (Time-dependent view from a single observer location) The Data Sets: IPS (STELab, Ooty, EISCAT), SMEI This Project: An inner heliospheric boundary

3. All sky ENA maps (Mollweide projection) for a SW-LISM interaction patterns.

4. Distribution of magnetic field strength in the meridional (z0x) and ecliptic (x0y) planes and the computational grid adapted to discontinuities in the solution of the SW–LISM interaction problem. The Sun is located within the bright red blob in the center of the figure.

5. 4065 eV 4065 eV 2558 eV 2558 eV 2558 eV 1726 eV 1726 eV 1726 eV North ecliptic pole ENAs (IBEX launch 2008 October 19)

6. 4065 eV 2558 eV 1726 eV South ecliptic pole ENAs (lBEX launch 2008 October 19)

7. STELab IPS Heliospheric Analyses DATA STELab IPS array near Fujioperating at 327 MHz

8. Current STELab IPS Heliospheric Analyses New STELab IPS array at Toyokawa - photo February 17, 2007 (new 327 MHz array now operates)

9. IHY - Other Currently Working IPS Radio Systems The Ootacamund (Ooty) off-axis parabolic cylinder 530 m long and 30 m wide (15,900 m2) operating at a nominal frequency of 326.5 MHz

10. IHY - Other Current IPS Radio Systems MEXART IPS 9,600 m2 140 MHz IPS radio array near Michoacan, Mexico

11. Scintillation Level Heliospheric Analysis Jackson, B.V., et al., 2009, Adv. in Geosciences (in press). Intensity interplanetary scintillation (IPS) g-levels. STELab IPS IPS line-of-sight response g = m/<m>

12. Heliospheric 3-D Reconstruction Jackson, B.V., et al., 2009, Adv. in Geosciences (in press). The outward-flowing solar wind structure follows very specific physics as it moves outward from the Sun LOS Weighting

13. Jackson, B.V., et al., 2009, Adv. in Geosciences (in press). The UCSD 3D-reconstruction program The “traceback matrix”(any solar wind model works)In the traceback matrix the location of the upper level data point (starred) is an interpolation in x of Δx2 and the unit x distance – Δx3 distance or (1 – Δx3). Similarly, the value of Δt at the starred point is interpolated by the same spatial distance. Each 3D traceback matrix contains a regular grid of values ΣΔx, ΣΔy, ΣΔt, ΣΔv, and ΣΔm that locates the origin of each point in the grid at each time and its change in velocity and density from the heliospheric model.

14. Heliospheric 3-D Reconstruction Jackson, B.V., et al., 2009, Adv. in Geosciences (in press). Line of sight “crossed” components on a reference surface. Projections on the reference surface are shown. These weighted components are inverted to provide the time-dependent tomographic reconstruction. 13 July 2000 14 July 2000

15. http://ips.ucsd.edu/ UCSD time-dependent IPS Web forecast Velocity model time-series G-level sky map Real-time tomographic analysis of the solar wind on April 29-30, 2004 showing a halo CME response in the interplanetary medium. Web Analysis Runs Automatically Using Linux on a P.C.

16. Tokumaru, M., et al., 2010, J. Geophys Res. (in press). “Solar cycle evolution of the solar wind speed from 1985-2008” (part of the result is shown here). The recently past solar minimum is pretty special in that there is a large variation of solar wind speed over solar latitude.

17. UCSD time-dependent IPS Velocity and density analysis (also at the CCMC) Density ecliptic cut Velocity ecliptic cut Tomographic analysis of the solar wind for Carrington rotation 2085 (2009/06/26 – 2009/07/23).

18. UCSD time-dependent IPS Velocity and density analysis (also at the CCMC) Density meridional cut Velocity meridional cut Tomographic analysis of the solar wind for Carrington rotation 2085 (2009/06/26 – 2009/07/23).

19. UCSD time-dependent IPS Velocity and density analysis (also at the CCMC) Density remote-observer view Velocity remote-observer view Tomographic analysis of the solar wind for Carrington rotation 2085 (2009/06/26 – 2009/07/23).

20. Other Ooty Density 3-D Reconstruction 4-7 November 2004 Bisi, M.M., et al., 2009, Annales Geophysicae, 27, 4479. The left shows an ecliptic cut through the 3D Ooty IPS density reconstruction and the right shows a meridional cut (from East of the Sun-Earth line) of the same; both with the Earth on the right-hand side and it’s orbit are shown.

21. Other Ooty Velocity 3-D Reconstruction 4-7 November 2004 Bisi, M.M., et al., 2009, Annales Geophysicae, 27, 4479. The left shows an ecliptic cut through the 3D Ooty IPS speed reconstruction and the right shows a meridional cut (from East of the Sun-Earth line) of the same; both with the Earth on the right-hand side and it’s orbit are shown.

22. Other Ooty 3-D Density and Velocity Reconstruction Bisi, M.M., et al., 2009, Annales Geophysicae, 27, 4479.

23. Other Bisi, M.M., et al., 2010,Solar Phys. (submitted). EISCAT Result Bisi, M.M., et al., 2010, Solar Phys., (submitted) It now becomes more important to be absolutely certain of the higher-frequency velocity LOS weighting.

24. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 Other 2003 May 27-28 CME events SMEI density 3D reconstruction of the 28 May 2003 halo CME as viewed from 15º above the ecliptic plane about 30º east of the Sun-Earth line. SMEI density (remote observer view) of the 28 May 2003 halo CME

25. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 2003 May 27-28 CME events Other CME masses

26. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 Other 27-28 May 2003 CME event period IPS Velocity and SMEI proton density reconstruction of the 27-28 May 2003 halo CME sequence. Reconstructed and Windin-situ densities are compared with over one Carrington rotation.

27. The best procedure is to obtain an inner heliosphere boundary of physical parameters, and using the best physics, extrapolate this outward to the largest distance possible. Hopefully, some variation in the inner solar wind will be manifest in the ENA flux observed at the interstellar boundary. In this way one can hope to learn more about the location of the ENA flux and also something about the shape of the interstellar boundary.

28. 4065 eV 2558 eV 1726 eV SW pressure North ecliptic pole ENAs (IBEX launch 2008 October 19)

29. 4065 eV 2558 eV 1726 eV SW pressure South ecliptic pole ENAs (lBEX launch 2008 October 19)

30. Summary: 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. There are several data sources (IPS, SMEI), but the most long-term and substantiated data source (that also measures velocity globally) is IPS data from the STELab arrays in Japan. Accurate observations of inner heliosphere parameters coupled withthe best physicscan extrapolate these outward to the interstellar boundary.