1. B.V. Jackson H.-S. Yu, P.P. Hick, A. Buffington,
Center for Astrophysics and Space Sciences,
University of California at San Diego, LaJolla, CA, USA
H.-S. Yu, P.P. Hick, A. Buffington,
Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA
Where necessary I will add comments
Masayoshi

2. Introduction:
IPS Space Weather Predictions, Heliospheric Visualizations
Plasma Parameters, D, V
Plasma Parameters, MAG
Driving 3D MHD analyses – ENLIL, others
Standardization of IPS Data Sets with In-situ Measurements
Low Resolution Faraday Rotation Depictions
Thomson Scattering Tomography
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3. IPS Space Weather Predictions

4. Yesterday’s Forecast Analysis
Where necessary I will add comments
Masayoshi

5. Today’s Forecast Analysis
Where necessary I will add comments
Masayoshi

6. Yesterday’s Forecast Analysis
Where necessary I will add comments
Masayoshi

7. Today’s Forecast Analysis
Where necessary I will add comments
Masayoshi

8. UCSD IPS prediction analysis
Skysweep view
Jackson, B.V., et al., 2011, Adv. in Geosciences, 30,
UCSD IPS prediction analysis
A Hammer-Aitoff display showing the STELab source locations. The source value is indicated relative to the model background value.
Web analysis runs automatically using Linux on a P.C.

9. IPS Space Weather Predictions

10. UCSD IPS prediction analysis
Skymap view
Jackson, B.V., et al., 2011, Adv. in Geosciences, 30,
UCSD IPS prediction analysis
Hammer-Aitoff sky maps of velocity and g-level (produced from the model).
Web analysis runs automatically using Linux on a P.C.

11. UCSD IPS prediction analysis
Skymap view
Jackson, B.V., et al., 2011, Adv. in Geosciences, 30,
UCSD IPS prediction analysis
“Fisheye” sky maps produced from the model.
Web analysis runs automatically using Linux on a P.C.

12. UCSD Kinematic IPS Model
IPS Prediction (KSWC)
UCSD Kinematic IPS Model

13. IPS Prediction (KSWC) IPS-Driven ENLIL
IPS-Driven ENLIL

14. Running the Program

15. bender:~/soft/for/development/ipstd20n_in-situ/test_3DMHD/v16a_test$
bender:~/soft/for/development/ipstd20n_in-situ/test_3DMHD/v16a_test$ ./ipstd_20n_inp_mag3_v16a_intel nagoya=nagoya.[4],,yearly nso_gorr=/home/bjackson/dat/gong/hcss/nso_gong[4]_[3].fts %ForeignArg-I-=, ======== %ForeignArg-I-Arg 1, nagoya=nagoya.[4],,yearly %ForeignArg-I-Arg 2, nso_gorr=/home/bjackson/dat/gong/hcss/nso_gong[4]_[3].fts %ForeignArg-I-=, ======== I, cVar(I) 1 nagoya=nagoya.[4],,yearly I, cVar(I) 2 nso_gorr=/home/bjackson/dat/gong/hcss/nso_gong[4]_[3].fts %MAP_TZERO-I-JDCar, Start yr 1985, doy (JD ) %MAP_TZERO-I-JDCar, End yr 2134, doy (JD ) Forecast mode? (YES/NO) < NO > Number of iterations? < 18 > Deconvolution distance (AU; 0=solar surface)? < -15 > Deconvolve: velocity, G-level, both? < both? > Use velocity data from: UCSD, EISCAT, Ooty, Nagoya, Gen,? < Nagoya > Minimum # of velocity lines of sight to use in the reconstruction? < 50 > Use in-situ velocity in the 3D reconstructions? (YES/NO) < YES > Use in-situ velocity from: ACE_L0, ACE_L2, Wind, CELIAS < Wind > Minimum velocity for in-situ velocity values? < 100 > Maximum velocity for in-situ velocity values? < 1500 > Use G-level data from: UCSD, Cambridge, Ooty, Nagoya, Gen,? < Nagoya > Minimum # of density lines of sight to use in the reconstruction? < 50 > Use in-situ density in the 3D reconstructions? (YES/NO) < YES > Use in-situ density from: ACE_L0, ACE_L2, Wind, CELIAS < Wind > Fit in-situ density data to Wind? (YES/NO) < YES > Minimum density for fit in-situ density values? < 0.1 > Maximum density for fit in-situ density values? < 200 > Fit mean g-level to Wind? (YES/NO) < YES >

16. Anti-Earth minimum density at 1 AU
Anti-Earth minimum density at 1 AU? < 2 > Please, select from range [90,180] Angular distance from Earth to begin D limit? < 135 > Please, select from range [0,180] Maximum RA relative to Sun for G-data? < 90 > G-map reference distance in AU (0=solar surface)? < E-2 > Do you want to use a proxy map for density? (YES/NO) < NO > Maximum limit for G deconvolution? < 4 > Minimum limit for G deconvolution? < 0.2 > Factor by which to modify g-level excursions? < 1 > G-level time hole filter? < 1 > Velocity time hole filter? < 1 > G-level spatial filter? < 14 > Velocity spatial filter? < 14 > G-level temporal filter? < > Velocity temporal filter? < > G-level power to fit density? < > AU average density to fit base? < 5 > G-level power to fit velocity? < > Radial G-level falloff to fit G density? < 0.2 > Radial G-level falloff to fit V density? < 0.2 > Solar wind speed for G-level traceback? < 400 > Map Extraction distance (AU; 0=solar surface)? < 1 > Please, select from range [ , ] Carrington rotation (0 = STOP)? < 2056 > # Intermediate rotations interpolated < 1 > # Rotations averaged < 1 > %MAP_TZERO-I-JDCar, Start yr 2007, doy (JD ) %MAP_TZERO-I-JDCar, End yr 2156, doy (JD ) Carrington rotation 2056 starts on date 27-APR-2007 ( Doy 117 ) Do you want to output model-source files? (YES/NO) < NO >

17. Faraday Rotation

18. One Use: Rotation Measure (Faraday rotation) skymaps to check heliospheric measurements

19. One Use: Rotation Measure (Faraday rotation) skymaps to check heliospheric measurements

20. One Use: Rotation Measure (Faraday rotation) skymaps to check heliospheric measurements

21. One Use: Rotation Measure (Faraday rotation) skymaps to check heliospheric measurements

22. Thomson Scattering

23. Heliospheric 3D-reconstructions
Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339
Heliospheric D-reconstructions
30º
LOS Weighting
60º
90º
The outward-flowing solar wind structure follows very specific physics as it moves outward from the Sun
Thomson scattering

24. SMEI Webpages - http://smei.ucsd.edu
Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi: /2008JA013224
27-28 May 2003 CME event period
The SMEI instrument was closed by the Air Force in September 2011, UCSD maintains the only SMEI Web pages and has upgraded them at: SMEI high resolution tomography has been used to reconstruct a filament at 1 AU!
Full SMEI data set, 6-hour cadence, 3º x 3º lat, long
SMEI proton density reconstruction for the May 2003 halo CME sequence. Reconstructed and ACE L2 in-situ densities are compared over one Carrington rotation.
SMEI Webpages - 24

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

26. SMEI High Resolution Tomography
The SMEI instrument was closed by the Air Force in September 2011, UCSD maintains the only SMEI Web pages and has upgraded them at: SMEI high resolution tomography has been used to reconstruct a filament at 1 AU!
A Filament Observed at 1 AU!
Sharma., et al., 2013, IAUS300 proceedings, (in press).
SMEI Webpages -

27. Summary: IPS Space Weather Predictions, Heliospheric Visualizations
Plasma Parameters, D, V
Plasma Parameters, MAG
Driving 3D MHD analyses – ENLIL, others
Standardization of IPS Data Sets with In-situ Measurements
Low Resolution Faraday Rotation Depictions
Thomson Scattering Tomography
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