1. H.-S. Yu1, B.V. Jackson1, P.P. Hick1,
ENLIL Driven by a Global Solar Wind Boundary from Remotely-Sensed IPS Data
H.-S. Yu1, B.V. Jackson1, P.P. Hick1,
A. Buffington1, M. M. Bisi2, D. Odstrcil3,4, M. Tokumaru5, J. Kim6, S. Hong6, B. Lee7, J. Yi7, J. Yun7
1CASS, UCSD, USA ; 2STFC RALab, Harwell Oxford, UK
3George Mason University & 4NASA/GSFC, United States
5ISEE, Nagoya, Japan
6KSWC, Jeju, South Korea, 7SELab, Seoul, South Korea

2. Introduction Data Sets - Interplanetary scintillation (IPS)
IPS data are mainly from ISEE (STELab), Japan
Analysis - 3D Heliospheric Tomography
fitting a kinematic model to the IPS data
(a time-dependent heliospheric view from a single observer location)
Speeds and densities from the IPS, vector fields from solar surface magnetograms
Current Applications:
A global solar wind boundary for driving 3D-MHD models
(UAH/MS-FLUKSS; NRL/H3D-MHD; ENLIL in real time)

3. (Same type of array located at Kiso) (Kiso, Mt. Fuji, and Toyokawa)
Interplanetary Scintillation (IPS) data – ISEE (STELab)
The STELab interplanetary scintillation 327 MHz remote-sensing cylindrical parabola near Mt. Fuji is shown. The array moves in declination to provide views of sources at different locations in the sky as they pass overhead. The other array of this type is at Kiso, to the north of Toyokawa.
IPS array near Mt. Fuji
(Same type of array located at Kiso)
IPS array systems
(Kiso, Mt. Fuji, and Toyokawa)

4. Interplanetary Scintillation (IPS) data – ISEE (STELab)
Berine is here
The Solar Wind Imaging Facility, Toyokawa (SWIFT) array is shown in the above photograph. B. Jackson is standing on the steps that take one to the antenna dipoles. The non-moving array is steerable in declination, providing views of radio sources as the transit the meridian above Japan.
IPS array in Toyokawa (3,432 m2 array now operates well – year-round operation began in 2011)

5. Interplanetary Scintillation (IPS) data – ISEE (STELab)
IPS is caused by the presence of density inhomogeneities in the solar wind that disturb the signal from point-like radio sources.
These produce intensity variations that, when projected onto Earth’s surface, make a pattern that travels away from the Sun with the solar wind speed.
The correlation of this pattern between different radio sites allows a determination of the solar wind outflow speed.
The “normalized scintillation level” (g-level) of an IPS radio source signal relative to a nominal average value allows a determination of the solar wind density.

6. Other Current Operating IPS Radio Systems
Other current operating IPS radio arrays are shown. The Puschino, Russia array is the largest IPS array currently in existence.
The Ootacamund (Ooty), India off-axis parabolic cylinder 530 m long and 30 m wide (15,900 m2) operating at a nominal frequency of MHz.
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).

7. Other and Potential Future IPS Radio 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)
Additional radio arrays that are used or can potentially be used for IPS are (from upper left clockwise), the MEXican ARray Telescope (MEXART); the Korean Space Weather Center (KSWC) radio array, Jeju; the LOw Frequency ARray (LOFAR), The Netherlands and Western Europe; and the Murchison Widefield Array (MWA), Western Australia.
(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.)

8. 3D Heliospheric Tomography
The 3D tomographic reconstruction basically proceeds by least-squares fitting a purely kinematic heliospheric solar wind model to the IPS LOS signal assuming radial outflow and enforcing conservation of mass and mass flux (Jackson et al., 1998).
The UCSD 3D-reconstructed heliospheric density, velocity, and vector magnetic fields are available, as standard, from 15 Rs out to 3.0 AU and can be extracted at any distance in between to provide inner boundary inputs to drive 3D-MHD forward modeling.
The IPS-derived boundaries contain both information of background solar wind and transient structures.

9. A Global Solar Wind Boundary for 3D-MHD models – H3D-MHD

10. 3D Heliospheric Tomography- 2011/09/24 CME Sequence
A pair of closely-spaced CMEs erupted from NOAA AR1302 in conjunction with an M7 strength solar flare.

11. 3D Heliospheric Tomography- 2011/09/24 CME Sequence

12. 9/26th Geomagnetic Storm Bz became sharply south at times
solar wind increase from 350km/s to over 700 km/s

13. UCSD IPS Analysis
(Yu et al., 2015)

14. UCSD IPS Analysis (1-day average) 0.93 0.93 date UT shock CME1 CME2

15. IPS driven 3D-MHD:
H3D-MHD (40 Rs, 5ox5o)
(Yu et al., 2015)

16. IPS driven 3D-MHD: H3D-MHD (1-day average)
shock
CME1
CME2
0.58
shock
CME1
CME2
0.73
date UT

17. A Global Solar Wind Boundary for 3D-MHD models – ENLIL

18. IPS driven 3D-MHD: ENLIL (0.1 AU, 4ox4o)
(Yu et al., 2015)

19. IPS driven 3D-MHD: ENLIL (1-day average)
shock
CME1
CME2
0.45
shock
CME1
CME2
0.90
date UT

20. CMEs in HI-1 images

21. CMEs in HI-1 images

22. H3D-MHD & ENLIL (6-hr average)
IPS driven 3D-MHD:
H3D-MHD & ENLIL (6-hr average)
H3D-MHD
Good fit in magnitude
WIND
Model
Density
ENLIL
Model
Velocity
Good fit in timing

23. IPS driven ENLIL: Space Weather at Rosetta Spacecraft

24. 2014-09-19 Rosetta plasma energy (IES data)
IPS driven ENLIL: Space Weather at Rosetta Spacecraft
Rosetta plasma energy (IES data)

25. IPS driven ENLIL: Space Weather at Rosetta Spacecraft
SOHO/LASCO HALO CME Sep.09, 2014
C2 Start Time:   00:06 UT C3 Start Time: 00:31-06:28 UT Type of CME: Asymmetric HALO CME — FRONTSIDE pa1:  064   pa2:  063      
Total Width:  360 degrees Velocity Measurements: C2: 5 points PA 064 C3: 12 points PA 064 Average through both fields:  km/sec
@ PA 064 Acceleration: m/sec^2
GOES reports a LDE M4.5 class X-ray flare at 23:12/00:29/01:31 UT from AR 12158

26. IPS driven ENLIL: Space Weather at Rosetta Spacecraft
SOHO/LASCO HALO CME Sep.10, 2014
C2 Start Time:   18:00 UT C3 Start Time: 18:06-22:30 UT Type of CME: Asymmetric HALO CME — FRONTSIDE pa1:  335   pa2:  334      
Total Width:  360 degrees Velocity Measurements: C2 2 points PA 335 C3 12 points PA 335 Average through both fields:  km/sec
@ PA 0335 Acceleration: m/sec^2
GOES reports a LDE X1.6 class X-ray flare at 17:21/17:45/18:20 UT from AR 12158

27. IPS driven ENLIL: Space Weather at Rosetta Spacecraft

28. IPS driven ENLIL: Space Weather at Rosetta Spacecraft

29. IPS driven ENLIL: Space Weather at Rosetta Spacecraft

30. IPS driven ENLIL: Space Weather at Rosetta Spacecraft

31. Real-time IPS-Derived Boundaries for 3D-MHD Model
Updated every 6 hours at: ftp://cass185.ucsd.edu/data/IPSBD_Real_Time/ENLIL/ascii_data
(Yu, H-S., et al., 2015, Solar Phys.; Jackson, B.V., et al., 2015, Space Weather)

33. IPS driven ENLIL in Real-Time
ENLIL run daily on a GMU test site by Dusan Odstrcil. See:

34. IPS driven ENLIL in KSWC
ENLIL run with a six hour cadence (planned) on the KSWC Website See:

35. Summary
The analysis of IPS data provides low-resolution global measurements of density and velocity with a time cadence of about one day for both density and velocity, and slightly longer cadences for some magnetic field components.
Evaluating the 3D reconstruction at a given spherical radius provides a “global solar wind lower boundary” which can then be extrapolated outward by 3D-MHD models.
The 3D-MHD simulation results using IPS boundaries as input compare fairly well with in situ measurements.
Real-time IPS boundary data for driving MHD model (ENLIL) are now available.