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B.V. Jackson , H-S Yu, P.P. Hick, A. Buffington, J.M. Clover

3-D Reconstruction of the Inner Heliosphere from Remote-Sensing and In-Situ Data: Tracing Magnetic Field Structure to near the Solar Surface. B.V. Jackson , H-S Yu, P.P. Hick, A. Buffington, J.M. Clover Center for Astrophysics and Space Sciences,

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B.V. Jackson , H-S Yu, P.P. Hick, A. Buffington, J.M. Clover

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  1. 3-D Reconstruction of the Inner Heliosphere from Remote-Sensing and In-Situ Data: Tracing Magnetic Field Structure to near the Solar Surface B.V. Jackson, H-S Yu, P.P. Hick, A. Buffington, J.M. Clover Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA Munetoshi Tokumaru Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan and Lan Jian Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA, USA Masayoshi http://smei.ucsd.edu/ http://ips.ucsd.edu/

  2. Introduction: The Motive: 3-D Analysis of the Inner Heliosphere – Measurement of Outward Plasma flow. 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: The analysis that includes in-situ data and a magnetic field trace to near the solar surface.

  3. Magnetic Field Traceback IPS Density Ecliptic cut EIT 195

  4. DATA STELab IPS Heliospheric Analyses IPS line-of-sight response STELab IPS array near Mt. Fuji STELab IPS array systems

  5. Density Turbulence • Scintillation index, m, is a measure of level of turbulence • Normalized Scintillation index, g = m(R) / <m(R)> • g > 1  enhancement in Ne • g  1  ambient level of Ne • g < 1  rarefaction in Ne (CourtesyofP.K.Manoharan) A scintillation enhancement with respect to the ambient wind identifies the presence of a region of increased turbulence/density and a possible CME along the line-of-sight to the radio source.

  6. Other Current 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 The Pushchino Radio Observatory 70,000 m2 110 MHz array, Russia (summer 2006) Now named the “Big Scanning Array of the Lebedev Physical Institute” (BSA LPI).

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

  8. Other Current IPS Radio Systems KSWC IPS 700 m2 327 MHz IPS radio 32 tile array, Jeju Island, South Korea

  9. Current STELab IPS Heliospheric Analyses New STELab IPS array at Toyokawa - photo February 17, 2007 (3,432 m2 array now operates well – year-round operation)

  10. Solar Wind Imaging Facility (SWIFT) • Large-Aperture Parabolic Reflector • 88m×39m×η=3432×η㎡ • Efficiency ηobs~0.65 • 192-Elements Phased Array in N-S Direction • Single Beam with a Steerable Range of 60 deg S-30 deg N • 1 Element = Combination of East and West λ/2-dipoles • Delay Correction ・Low-Noise Receiver • 327MHz ±5MHz max • Front-end: NF <1dB、VSWR <1.5 • Loop-Method Calibration System • RFI Reduction • Small Height of Focal Points • Shielding Fence at North and South Ends North South

  11. Jackson, B.V., et al., 2012, Adv. in Geosciences (in press) Potential future IPS systems MWA (Western Australia) LOFAR (Western Europe) (32 tiles are now operating. The full array 128 tiles can obtain IPS.) (Some parts of the system are now operating - Richard Fallows, Mario Bisi, are involved. IPS/FR tests are ongoing) KSWC (Korea) *AOGS Special Session*ST25 – Singapore 13-17 August “Forecasting Solar Wind Parameters at the Earth and Planets”(B. Jackson, T. Nagatsuma, M. Tokumaru, P.K. Manoharan, M. Bisi, conveners) (Tiles ~like those of MWA are being used. So far a small system is deployed)

  12. Heliospheric 3-D Reconstruction Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, 339 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., 2008, Adv. in Geosciences, 21, 339. 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., 2008, Adv. in Geosciences, 21, 339. 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. IPS C.A.T. Analysis Jackson, B.V., et al., 2002, Solar Wind 10, 31 Bastille Day Event 14 July 2000 IPS Density Remote View

  16. IPS C.A.T. Analysis Jackson, B.V., et al., 2002, Solar Wind 10, 31 Bastille Day Event 14 July 2000 IPS Density Ecliptic Cut

  17. IPS C.A.T. Analysis Jackson, B.V., et al., 2002, Solar Wind 10, 31 Bastille Day Event 14 July 2000 IPS Velocity Ecliptic Cut

  18. IPS C.A.T. Analysis Jackson, B.V., et al., 2002, Solar Wind 10, 31 Bastille Day Event 14 July 2000 IPS Density Meridional Cut IPS Density LOS X-ing Meridional Cut

  19. Zhao, X. P. and Hoeksema, J. T., 1995, J. Geophys. Res., 100 (A1), 19. http://ips.ucsd.edu/ Magnetic Field Extrapolation Dunn et al., 2005, Solar Physics 227: 339–353. • Inner region: the CSSS model calculates the magnetic field usingphotospheric measurements and a horizontal current model. 2. Middle region: the CSSS model opens the field lines. In the outer region. 3. Outer region: the UCSD tomography convects the magnetic field along velocity flow lines. Jackson, B.V., et al., 2012, Adv. in Geosciences (in press)

  20. IPS C.A.T. Analysis Dunn, T.J., et al., 2005, Solar Phys., 227, 339 Potential field modeling added IPS Density Remote View

  21. Heliospheric 3D-reconstructions Jackson, B.V., et al., 2012, Adv. in Geosciences, (in press). CR2056 Radial Field Tangential Field Normal Field NSO Data

  22. Heliospheric 3D-reconstructions Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256. Lan Jian CCMC Study In-SituTomographic analysis

  23. Heliospheric 3D-reconstructions Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256. Lan Jian CCMC Study In-SituTomographic analysis

  24. Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256. IPS line-of-sight response Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, 339. Heliospheric C.A.T. Analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction. Innovation STELab IPS * 13 July 2000 Inclusion of in-situ measurements into the 3D-reconstructions

  25. Heliospheric 3D-reconstructions Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256. Innovation Innovation Inclusion of in-situ measurements into the 3D-reconstructions Jackson, B.V., et al., 2008, Adv. in Geosciences, (in press).

  26. Heliospheric 3D-reconstructions CR2056 Jackson, B.V., et al., 2010, Solar Phys., 265, 245-256. Velocity Jackson, B.V., et al., 2012, Adv. in Geosciences, (in press). Density

  27. Heliospheric 3D-reconstructions Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256. Being evaluated at the CCMC Jackson, B.V., et al., 2012, Adv. in Geosciences, (in press). Forecast Density Forecast Forecast Inclusion of in-situ measurements into the 3D-reconstructions Forecasts work better if the values match up to the present. Velocity Forecast

  28. Heliospheric 3D-reconstructions Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256. Being evaluated at the CCMC Jackson, B.V., et al., 2012, Adv. in Geosciences, (in press). Forecast Density Density Forecast Inclusion of in-situ measurements into the 3D-reconstructions Forecasts work better if the values match up to the present. Velocity Velocity Forecast

  29. Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256. Jackson, B.V., et al., 2012, Adv. in Geosciences, (in press). CCMC Forecast Presentation Velocity Forecast Density

  30. Jackson, B.V., et al., 2012, Adv. in Geosciences, (in press). http://ips.ucsd.edu/ UCSD Web pages UCSD IPS analysis Web Analysis Runs Automatically Using Linux on a P.C.

  31. Jackson, B.V., et al., 2012, Adv. in Geosciences, (in press). http://ips.ucsd.edu/Earth Velocity and Density Web Analysis Runs Automatically Using Linux on a P.C.

  32. Jackson, B.V., et al., 2012, Adv. in Geosciences, (in press). http://ips.ucsd.edu/Earth Radial and Tangential Magnetic Field Web Analysis Runs Automatically Using Linux on a P.C.

  33. Jackson, B.V., et al., 2012, Adv. in Geosciences, (in press). http://ips.ucsd.edu/ Density overview UCSD IPS analysis Web Analysis Runs Automatically Using Linux on a P.C.

  34. Magnetic Field Traceback Traceback Matrix IPS Velocity Ecliptic cut Zhao, X. P. and Hoeksema, J. T., 1995, J. Geophys. Res., 100 (A1), 19. Dunn, T., et al., 2005, Solar Phys., 227, 339–353. Jackson, B.V., et al., 2012, Adv. in Geosciences (in press)

  35. Magnetic Field Traceback EIT 195 ACE Ion data 2007/05/08 IPS Velocity Ecliptic cut

  36. 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, and slightly longer cadences for some magnetic field components. There are several near real time and archival 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 Earth or the interstellar boundary.

  37. Heliospheric 3D-reconstructions Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256. Lan Jian CCMC Study In-SituTomographic analysis

  38. Heliospheric 3D-reconstructions Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256. Lan Jian CCMC Study In-SituTomographic analysis

  39. Jackson, B.V., et al., 2012, Solar Phys., (under review). Density analysis for all of CR 2114 IPS time series – time of tomographic run compared to ACE one day in advance Correlation

  40. Jackson, B.V., et al., 2012, Solar Phys., (under review). Analysis CR 2110 – CR 2116 (spring – winter 2011) IPS time series compared to ACE

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