CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San.

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CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA Masayoshi P.P. Hick, A. Buffington, H.-S. Yu, Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA D. Odstrcil George Mason University, Fairfax, Virginia, and NASA-Goddard Spaceflight Center, USA With help from M. Tokumaru, M. Kojima Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya , Japan (STELab foreign visitor fund)

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models IPS Advances: Dedicated IPS Systems: STEL (ISEE), Japan; MEXART, Mexico; KSWC, Jeju; Pushchino, Russia; Ooty, India(?) Interesting Developments: Chinese IPS An IPS standard data format Pushchino source data availability Space Weather Special Issue Next IPS workshop An Iterative 3D-MHD IPS Analysis: Progress so far Work needed Introduction:

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models World-Wide IPS observation network Japan Mexico India Russia UK/EISCAT LOFAR) US-Australia Ooty 327MHz 、 16,000 ㎡ Pushchino103MHz 70,000 ㎡ MEXART 140MHz 、 10,000 ㎡ MWA MHz STEL Multi-Station 327MHz 2000 ㎡ ×2, 3500 ㎡ (Toyokawa) IPS Korea Miyun, China 327,611,2300,8400MHz ~1100 ㎡

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models “Dedicated” IPS Systems

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models STELab IPS array near Mt. Fuji 327 MHz ~2000 ㎡ DATA STELab IPS array systems IPS Heliospheric Analyses (STELab) Toyokawa IPS array 327 MHz ~3500 ㎡

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Current Dedicated IPS Radio Systems The Pushchino Radio Observatory 70,000 m MHz array, Russia (summer 2006) Now named the “Big Scanning Array of the Lebedev Physical Institute” (BSA LPI). The Ootacamund (Ooty), India off-axis parabolic cylinder 530 m long and 30 m wide (15,900 m 2 ) operating at a nominal frequency of MHz.

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Other and Potential Future Dedicated IPS Systems MEXART (Mexico) KSWC (South Korea) Dedicated IPS 700 m MHz IPS radio 32 tile array, Jeju Island Dedicated IPS IPS 9,600 m MHz IPS radio array near Michoacan, Mexico

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Interesting IPS Developments

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Third Remote-Sensing Workshop October 2015 Morelia, Mexico

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Morelia Wks. - IPS in China Urumqi (Xinjiang Astronomical Obs.) First SSSF IPS observing station in China Diameter : 25m Wavelength: 18cm ( cm) Miyun (National Astronomical Obs.) Diameter : 50m Frequency: 327, 611, 2300, 8400MHz IPS group in JLRAT, NAOC

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Standard IPS Format Date MidObsUT Dur. Site Freq BW Source Size RA-J2000 Dec-J2000 Limb Dist. Lat. PA Elong Vel. V-err g-value g-err Method Vel. V-err g-value g-err Method :57: STEL C E St. CC St. PS Date MidObsUT Dur. Site Freq BW Source Size RA-J2000 Dec-J2000 Limb Dist :57: STEL C E Lat. PA Elong Vel. V-err g-value g-err Method Vel. V-err g-value g-err Method St. CC St. PS Ascii – Fixed Format As: ftp://ftp.stelab.nagoya-u.ac.jp/pub/vlist/STEL2015.dat G-value, error New item Used by UCSD tomo.

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Pushchino Data Availability ° declination

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Space Weather Special Issue Mid-February announcement Guest Editors: Mario Bisi Bernie Jackson Igor Chasei

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models IPS Workshop UCSD, San Diego ~18-20 (Sunday-Tuesday) December 2016 (following the San Francisco fall AGU)

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models More Details An Iterated IPS Time-Dependent 3D-MHD Model

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Sample outward motion over time Heliospheric C.A.T. analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction. IPS line-of-sight response Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, STELab IPS

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models 13 July July 2000 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 IPS line-of-sight response Jackson, B.V., et al., 2008, Adv. in Geosciences, 21,

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models IPS Prediction (KSWC) (a couple years ago)

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Fisheye velocity skymaps with additional radio sources Time-Dependent Analysis Using Other IPS Systems Analysis including MEXART source Analysis without MEXART source Jackson, B.V., et al., 2013, AGU 2013 Presentation, May, Cancun, Mexico. (Speed the same as at STELab)

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models IPS-Derived 3D-MHD Model Boundaries (Yu, H-S., et al., et al., 2015, Solar Phys., doi: /s ) (Jackson, B.V., et al.,., 2015, Space Weather, 13, doi: / /803/1/L1.) Updated every 6 hours at: ftp://cass185.ucsd.edu/data/IPSBD_Real_Time/ENLIL/ascii_data

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Velocity Shock & CME ENLIL IPS H3DMHD UCSD kinematic model and IPS-driven 3D-MHD models

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Density Shock & CME ENLIL IPS H3DMHD UCSD kinematic model and IPS-driven 3D-MHD models

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models IPS Boundaries used to drive ENLIL in Real Time (Yu, H-S., et al., 2015, Solar Phys., doi: /s ) (Jackson, B.V., et al., 2015, Space Weather, 13, doi: / /803/1/L1.) ENLIL run daily on a GMU test site by Dusan Odstrcil. See:

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models 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. The UCSD 3D-reconstruction program Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, Traceback Using an External Volume

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models 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. The UCSD 3D-reconstruction program Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, Traceback Using an External Volume don’t The “traceback matrix” (any solar wind model works) If you don’t have a model, then you can go from the lower level outward and conserve mass and mass flux at each outward step as in the UCSD kinematic time-dependent model analysis.

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models don’t The “traceback matrix” (any solar wind model works) If you don’t have a model, then you can go from the lower level outward and conserve mass and mass flux at each outward step as in the UCSD kinematic time-dependent model analysis. The UCSD 3D-reconstruction program Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, Traceback Using an External Volume do The “traceback matrix” (any solar wind model works) If you do have a model, then you can go from the outmost level downward, tracing the location of each point in the regular grid to the lower level below it until you get to the lowest level in the volume. In this way any model allows the traceback. So what is needed is to present each volume to the tomography program in the tomographic program coordinate system – namely in corotating heliographic coordinates and at the temporal resolution of the tomography.

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models Traceback from an external model. Files read from and external model now works. Integration into the UCSD tomography program (discuss magnetic field integration). Conversion of a given external volume into the corotating UCSD heliographic coordinate system. Tests of the 3D-MHD iterative analyses. Iterated IPS Time-Dependent Tomography to Date:

CASS/UCSD STEL 2016 Iterated Time-dependent IPS 3D-MHD Models IPS Advances: Dedicated IPS Systems: STEL (ISEE), Japan; MEXART, Mexico; KSWC, Jeju; Pushchino, Russia; Ooty, India(?) Interesting Developments: Chinese IPS An IPS standard data format Pushchino source data availability Space Weather Special Issue Next IPS workshop An Iterative 3D-MHD IPS: Progress so far Work needed Summary: