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 http://ips.ucsd.edu/ Where necessary I will add comments Masayoshi

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 My talk will proceed this way

IPS Space Weather Predictions

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

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

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

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

UCSD IPS prediction analysis http://ips.ucsd.edu/ Skysweep view Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115. 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.

IPS Space Weather Predictions

UCSD IPS prediction analysis http://ips.ucsd.edu/ Skymap view Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115. 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.

UCSD IPS prediction analysis http://ips.ucsd.edu/ Skymap view Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115. UCSD IPS prediction analysis “Fisheye” sky maps produced from the model. Web analysis runs automatically using Linux on a P.C.

UCSD Kinematic IPS Model IPS Prediction (KSWC) http://www.spaceweather.go.kr/models/ips UCSD Kinematic IPS Model

IPS Prediction (KSWC) IPS-Driven ENLIL http://www.spaceweather.go.kr/models/ips IPS-Driven ENLIL

Running the Program

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 24.622 (JD 2446090.1) %MAP_TZERO-I-JDCar, End yr 2134, doy 126.91 (JD 2500613.4) 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 >

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)? < 6.97861004E-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? < 0.64999998 > Velocity temporal filter? < 0.64999998 > G-level power to fit density? < 0.34999999 > 1 AU average density to fit base? < 5 > G-level power to fit velocity? < 0.34999999 > 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 [1757.88,2184.18] Carrington rotation (0 = STOP)? < 2056 > # Intermediate rotations interpolated < 1 > # Rotations averaged < 1 > %MAP_TZERO-I-JDCar, Start yr 2007, doy 8.495 (JD 2454109) %MAP_TZERO-I-JDCar, End yr 2156, doy 110.848 (JD 2508632.3) Carrington rotation 2056 starts on date 27-APR-2007 ( Doy 117 ) Do you want to output model-source files? (YES/NO) < NO >

Faraday Rotation

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

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

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

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

Thomson Scattering

Heliospheric 3D-reconstructions Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339 Heliospheric 3D-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

SMEI Webpages - http://smei.ucsd.edu Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 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: http://smei.ucsd.edu. 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 27-28 May 2003 halo CME sequence. Reconstructed and ACE L2 in-situ densities are compared over one Carrington rotation. SMEI Webpages - http://smei.ucsd.edu 24

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

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: http://smei.ucsd.edu. 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 - http://smei.ucsd.edu

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 M Potentaily talk will proceed this way