1. IPS Heliospheric Analyses (STELab)
DATA
IPS Heliospheric Analyses (STELab)
STELab interplanetary scintillation 327 MHz remote-sensing of the interplanetary medium is shown. <click> Density inhomogenieties in the solar wind on the order of 150 km size from point radio sources produce an intensity pattern variation on the ground that 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.
IPS line-of-sight response
STELab IPS array near Mt. Fuji
STELab IPS array systems

2. Current STELab Toyokawa IPS System
New STELab IPS array in Toyokawa (3,432 m2 array now operates well – year-round operation began in 2011)

3. IPS line-of-sight response
Jackson, B.V., et al., 2008, Adv. in Geosciences, 21,
Heliospheric C.A.T. analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction.
STELab IPS
The same is shown for daily observations from STELab IPS observations. <click> For the IPS, the “Nagoya” line of sight weighting provides a weight for each source observation on the source surface.
14 July 2000
13 July 2000

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

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

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

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

8. Magnetic Field Extrapolation
Zhao, X. P. and Hoeksema, J. T., 1995, J. Geophys. Res., 100 (A1), 19.
Magnetic Field Extrapolation
Inner region: the CSSS model calculates the magnetic field using photospheric 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.
Dunn et al., 2005, Solar Physics 227: 339–353.
Jackson, B.V., et al., 2012, Adv. in Geosciences, 30,

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

10. IPS line-of-sight response
Jackson, B.V., et al., 2010, Solar Phys., 265,
IPS line-of-sight response
Jackson, B.V., et al., 2010, Adv. in Geosciences, 21,
Jackson, B.V., et al., 2012, Solar Phys. published on-line.
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
The same is shown for daily observations from STELab IPS observations. <click> For the IPS, the “Nagoya” line of sight weighting provides a weight for each source observation on the source surface. *
13 July 2000
Inclusion of in-situ measurements into the 3D-reconstructions

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

12. Heliospheric 3D-reconstructions
Jackson, B.V., et al., 2010, Solar Phys., 265,
Jackson, B.V., et al., 2011, Adv. in Geosciences, 30,
Forecast
Jackson, B.V., et al., 2012, Solar Phys. published on-line.
Heliospheric 3D-reconstructions
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

13. Heliospheric 3D-reconstructions
Jackson, B.V., et al., 2010, Solar Phys., 265,
Jackson, B.V., et al., 2011, Adv. in Geosciences, 30,
Forecast
Jackson, B.V., et al., 2012, Solar Phys. published on-line.
Heliospheric 3D-reconstructions
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

14. Web Analysis Runs Automatically Using Linux on a P.C.
Jackson, B.V., et al., 2011, Adv. in Geosciences, 30,
UCSD Web pages
UCSD IPS forecasts
Web Analysis Runs Automatically Using Linux on a P.C.

15. Other and Potential Future IPS systems
MEXART (Mexico)
KSWC (South Korea)
Dedicated IPS 700 m2 327 MHz IPS radio 32 tile array, Jeju Island
Dedicated IPS IPS 9,600 m2 140 MHz IPS radio array near Michoacan, Mexico
MWA (Western Australia)
LOFAR (Western Europe)
(32 tiles are now operating. The full array 128 tiles can obtain some IPS data.)
(Some parts of the system are now operating - Richard Fallows, Mario Bisi are involved. IPS/FR tests are ongoing.)

16. Faraday rotation signals at low frequency
Oberoi and Lonsdale, 2012, Radio Science, 47, RS0K08, doi: /2012RS
Faraday rotation signals at low frequency
‗ ‗ Φ = λ2 ∫ neB•ds
From Oberoi and Lonsdale

17. Faraday rotation tomography
Future
Jackson, B.V., et al., 2008, URAS Workshop
‗ ‗ Φ = λ2 ∫ neB•ds
Jensen, E.A., et al., 2010, Solar Phys., 265, 31
Faraday rotation tomography
On the left is the Rotation Measure (RM) shown for with background magnetic field extrapolated from the solar surface to provide the FR signal (from the densities reconstructed during the Bastille Day CME). On the right is the same density but with the magnetic loop observed in ACE for this CME added to the IPS 3D reconstructed velocity to provide a sky map of Faraday rotation. The minimum signal from the MWA (expected to be a few degrees at 100MHz or ~3m) should be adequate to reconstruct this loop using the signals obtained from these RM measurements provided there are enough lines of sight covering the sky throughout the period of observation. The density loop and the magnetic loop (2 giant heliospheric loops systems) derived from these two very different 3D reconstruction techniques are not superimposed for this event.
Background Field, 3D UCSD Density
Background Field, 3D UCSD Density, Mulligan “Can”

18. Summary: The Future is here:
Forecasts with the IPS data (this has worked with STELab data for about 12 years).
Forecasts in real-time work better now with the inclusion of in-situ data (has been available since spring, 2011) These new innovations and the inclusion of other world IPS data sets make the technique a competitive way to measure velocities and densities.
FR inversion to obtain vector fields may work, but needs to be incorporated with a robust method of determining density to back out accurate vector magnetic fields remotely.