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Slides For A Possible CCMC Presentation 2013

Introduction:. Slides For A Possible CCMC Presentation 2013. Introduction:. Current IPS Systems IPS Advantage: Measures CMEs and corotating structures on their way to Earth Disadvantages: All arrays must map sources near their zenith, thus no information is available continuously.

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Slides For A Possible CCMC Presentation 2013

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  1. Introduction: Slides For A Possible CCMC Presentation 2013

  2. Introduction: Current IPS Systems IPS Advantage: Measures CMEs and corotating structures on their way to Earth Disadvantages: All arrays must map sources near their zenith, thus no information is available continuously. Single-site arrays produce less reliable IPS velocities than multi-site arrays. Small radio arrays provide information from only a few radio sources.

  3. Currently Dedicated IPS Radio Systems The Ootacamund (Ooty), India off-axis parabolic cylinder 530 m long and 30 m wide (15,900 m2) operating at a nominal frequency of 326.5 MHz. New STELab IPS array in Toyokawa (3,432 m2 array now operates well – year-round operation began in 2011) Scintillation (Radio source passing array beam)

  4. 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 along the line-of-sight to the radio source.

  5. IPS Heliospheric Analyses (STELab) Current STELab IPS System IPS line-of-sight response STELab IPS array near Mt. Fuji STELab IPS array systems

  6. World-Wide IPS observation network Pushchino103MHz 70,000㎡ STEL Multi-Station 327MHz 2000 ㎡×3, 3500 ㎡ MEXART 140MHz、10,000㎡ IPS UK/EISCAT LOFAR) Russia Korea Japan India Mexico MWA 80-300MHz Ooty 327MHz、16,000㎡ US-Australia

  7. Currently-Operated Dedicated IPS Radio Systems New STELab IPS 327 MHz array in the Toyokawa System (3,432 m2 array now operates well – year-round operation began in 2011)

  8. Single-site array Ooty, India Currently-Operated Dedicated IPS Radio Systems The Ootacamund (Ooty), India off-axis parabolic cylinder 530 m long and 30 m wide (15,900 m2) operating at a nominal frequency of 326.5 MHz.

  9. Currently-Operated Dedicated IPS Radio Systems 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).

  10. Currently-Operated Dedicated IPS Radio Systems The MEXART Array, Near Morelia, Mexico. Operates at 140 MHz. Half of the 9,600 m2 area is now being used. The KSWC Array, Jeju, South Korea. Operates at 327 MHz. A small 32-tile system is being used. Estimate ~ 500 m2 area.

  11. Other Potential Future IPS systems LOFAR (Western Europe) Richard Fallows Some parts of the large multi-site multi-frequency 10 – 190 MHz system are now operating - Richard Fallows, Mario Bisi are involved. IPS/FR tests are ongoing.

  12. Other Potential Future IPS systems MWA (Western Australia) 128 tiles are now operating. The system has the potential to obtain multi-frequency (50- 240 MHz IPS data, but this has not been tried so far.

  13. Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115. Jackson, B.V., et al., 2013,Solar Phys., 285, 151-165. http://ips.ucsd.edu/ UCSD IPS WebPages UCSD IPS forecasts using STELab data Web Analysis Runs Automatically Using Linux on a P.C.

  14. Time-Dependent Analysis Using Other IPS Systems IPS tomography with additional radio sources can be provided at times intermediate to a one-day cadence. The following case shows the insertion of an IPS source velocity from MEXART single-site analysis into what was primarily the STELab IPS UCSD 327 MHz kinematic tomography. The MEXART IPS velocity (that in this instance was nearly identical but intermediate in time to that from STELab) from 140 MHz data was inserted with appropriate line-of sight weighting for that frequency.Little change in the result is observed, as is appropriate in this instance. If a fast CME had erupted following the STELab observations it could have been “caught” by the IPS tomography.

  15. Time-Dependent Analysis Using Other IPS Systems Fisheye velocity skymaps with additional radio sources Analysis including MEXART source Analysis without MEXART source

  16. Other fittings – Other times Mejia-Ambriz, J., et al., 2013, AGU 2013 Presentation , May, Cancoon, Mexico. Solar wind speeds measured by IPS model fitting using the same source (3C48) during April 2009. MEXART STEL (SWIFT) Mejia-Ambriz, J., et al., 2013, AGU 2013 Presentation , May, Cancoon, Mexico.

  17. Comparison Mejia-Ambriz, J., et al., 2013, AGU 2013 Presentation , May, Cancoon, Mexico. ● Fitting technique using: MEXART (◊) and STEL-SWIFT (∆). ● Multi-station technique with STEL stations (*). Time lags of the diffraction patterns propagating between separate stations. Mejia-Ambriz, J., et al., 2013, AGU 2013 Presentation , May, Cancoon, Mexico.

  18. Comparison between IPS Spectrum Fitting and Multi-Site Cross Correlation Velocity Methods from IPS obs. for 3C273 in 2012 3C273 2012/9/3 Correlation ~0.47 V1st/V3st=1.04±0.24 V1st. (km/s) V3st. (km/s) Cross Correlation Method (3-station meas.) Speed V3st.= 457±13 km/s Spectrum Fitting Method (Single-station meas.) Speed V1st.=459km/s Axial Ratio=1.07 Spectral Index=3.8 (Courtesyof M.Tokumaru) Tokumaru, M., et al., 2013, AOGS 2013 Presentation , June, Brisbane, Australia.

  19. (See Jackson, B.V., et al., 2013,Solar Phys., 285, 151-165.) To Make a 3D-MHD Boundary Time-Dependent Velocity at 0.25 AU IHG Coordinates

  20. (See Jackson, B.V., et al., 2013,Solar Phys., 285, 151-165.) To Make a 3D-MHD Boundary Time-Dependent Density at 0.25 AU IHG Coordinates

  21. (See Jackson, B.V., et al., 2013,Solar Phys., 285, 151-165.) To Make a 3D-MHD Boundary Time-Dependent Radial Field at 0.25 AU, IHG Coordinates

  22. ENLIL WSA-GONG 3D-MHD 2011/08 to 2011/09 CASE STUDY ENLIL 3D-MHD modeling using WSA-GONG inputs3D time-dependent IPS tomography boundary. (Recent Work) Period on 26 September (center of plots) is an interesting example

  23. ENLIL IPS Boundary 3D-MHD 2011/08 to 2011/09 CASE STUDY (Also see Jackson, B.V., et al., 2013,Solar Phys., 285, 151-165.) ENLIL 3D-MHD modeling using a 21.5 Rs 3D time-dependent IPS tomography boundary. (Recent Work) Period on 26 September (center of plots) is an interesting example (Dusan, why didn’t you use the UCSD |B| inputs?) Analysis Can Run Automatically Using Linux on a P.C.

  24. Other IPS Boundary 3D-MHD Ooty IPS velocities and g-level densities.C.C. Wu HAF 3DMHD modeling from an 18 Rs 3D time-dependent IPS tomography boundary. (Wu, S.T., et al., 2001, J. Geophys. Res. 106, 25089-25102.) 3D-MHD 3D-MHD HAF 3DMHD

  25. Other IPS Boundary 3D-MHD MS-FLUKSS 3D-MHD modeling from a 0.25AU 3D time-dependent IPS tomography boundary. (Kim, T. K., 2012, AIP Conference Proc. 1500, pp. 140-146.)

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