AOGS2008 Busan South Korea

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IAU-JD16-WHI Rio de Janeiro, Brazil invited
3D Reconstructions of the Whole Heliosphere
Interval and Comparison with in-Ecliptic Solar
Wind Measurements from STEREO, ACE, and Wind
Instrumentation
Mario M. Bisi1 (mmbisi_at_ucsd.edu), Bernard V.
Jackson1, John M. Clover1, P. Paul Hick1, Andrew
Buffington1, and M. Tokumaru2.

• 1Center for Astrophysics and Space Sciences
  (CASS), University of California, San Diego
  (UCSD), 9500 Gilman Drive 0424, La Jolla, CA
  92093-0424, U.S.A.
• 2Solar-Terrestrial Environment Laboratory
  (STELab), Nagoya University, Furo-cho,
  Chikusa-ku, Nagoya 464-8601, Japan

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STELab IPS Arrays
The Solar-Terrestrial Environment Laboratory
(STEL/STELab) interplanetary scintillation (IPS)
arrays, Japan.
The STELab antennas from left-to-right Fuji,
Sugadaira, Toyokawa (old), and Kiso. (Courtesy of
http//stesun5.stelab.nagoya-u.ac.jp/uhf_ant-e.htm
l)
New STELab Toyokawa IPS array
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Outline

• Interplanetary Scintillation (IPS)
• Three-Dimensional (3D) Reconstructions
• 3D Reconstructions of STELab IPS data during the
  Whole Heliosphere Interval (WHI) and their
  comparison with various spacecraft
  measurements/observationsApril/May 2008
  (Carrington rotation CR2068)
• Summary
• Future Prospects

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Interplanetary Scintillation (1)
IPS is only sensitive to the component of flow
that is perpendicular to the line-of-sight By
suitably transforming and calibrating the
intensity scintillation time series, the solar
wind speed can also be obtained from the spectrum
of a single-site IPS observation
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Interplanetary Scintillation (2)
Different baselines can be used depending on the
geometry of the IPS raypath generally, the
largest cross-correlation occurs when the
baseline is close to the radial direction (R),
but not along the radial direction.
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Interplanetary Scintillation (3)
The velocity resolution improves as Bpar
(parallel baseline) increases but the correlation
decreases as turbulence evolves so the
correlation decreases need to have a balance
between the two.
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Interplanetary Scintillation (4)

• Density Turbulence
• Scintillation index, m, is a measure of level of
  turbulence
• Normalized Scintillation index, g m(R) / ltm(R)gt
• g gt 1 ? enhancement in ?Ne
• g ? 1 ? ambient level of ?Ne
• g lt 1 ? rarefaction in ?Ne

(Courtesy ofP.K. Manoharan)
Scintillation enhancement with respect to the
ambient wind identifies the presence of a region
of increased turbulence/density and possible CME
along the line-of-sight to the radio source
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Three-Dimensional (3D) Reconstructions (1)
STELab IPS
Heliospheric C.A.T. Analyses example
line-of-sight distribution for each sky location
to form the source surface of the 3D
reconstruction.
13 July 2000
14 July 2000
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Three-Dimensional (3D) Reconstructions (2)
Heliospheric C.A.T. Analyses velocity IPS
line-of-sight distribution during CR2068 for
each sky location plotted onto a Carrington
source-surface map (left).
Heliospheric C.A.T. Analyses line-of-sight
weighting values for each sky location (right).
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Time Period Discussed Here
Whole Heliosphere Interval (CR2068)
2008/03/20-2008/04/16 STELab IPS observations
commenced 2008/04/03 and were interrupted
againfor some time from 2008/04/22
- Bisi, M.M., B.V. Jackson, A. Buffington, J.M.
Clover, P.P. Hick, and M. Tokumaru,
Low-Resolution STELab IPS 3D Reconstructions of
the Whole Heliosphere Interval and Comparison
with in-Ecliptic Solar Wind Measurements from
STEREO and Wind Instrumentation, Solar Physics,
STEREO Science Results at Solar Minimum
Special Edition, doi10.1007/s11207-009-9350-9,
2009
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STELab IPS Synoptic Coverage of Velocity
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STELab IPS Lines of Sight g-level Observations
(Source Surface)
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STELab IPS Lines of Sight Velocity Observations
(Source Surface)
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STELab IPS Reconstructed Synoptic Coverage
(1 AU)
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STELab IPS WHI Density Reconstruction (1)
STELab IPS density reconstruction as seen in the
ecliptic plane for CR2068 when data were
available showing Earth and the two STEREO
spacecraft
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STELab IPS WHI Density Reconstruction (2)
STELab IPS density reconstruction as seen in the
meridional plane for CR2068 when data were
available showing Earth and its orbit across the
ecliptic
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STELab IPS WHI Speed Reconstruction (1)
STELab IPS speed reconstruction as seen in the
ecliptic plane for CR2068 when data were
available showing Earth and the two STEREO
spacecraft
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STELab IPS WHI Speed Reconstruction (2)
STELab IPS speed reconstruction as seen in the
meridional plane for CR2068 when data were
available showing Earth and its orbit across the
ecliptic
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CIR 04-06 April 2008
Ecliptic cut extractions from the 3D tomography
looking down from North of the ecliptic in both
density (top) and velocity (bottom) A period of
three days is shown here, centred on 0300UT for
each of the days
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CME 12-15 April 2008
Ecliptic cut extractions from the 3D tomography
looking down from North of the ecliptic in both
density (top) and velocity (bottom) A period of
four days is shown here, centred on 0300UT for
each of the days
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STEREO-B in situ Comparison
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Wind in situ Comparison
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ACE (level-0) in situ Comparison
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STEREO-A in situ Comparison
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Time Period Discussed Here Summary
CIR and CME features simultaneously early
on? CIR in speed and CME in density from the in
situ measurements and the 3D reconstructions tend
to agree (but g-level observations are too few to
the West particularly early in this time period
i.e. in the direction of STEREO-A)? What
about the STEREO HIs?
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STEREO HI Movies the whole of WHI
(Original images courtesy of Jackie Davies, RAL)
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STEREO-B Brightness Comparison
Only the STELab IPS time period is compared here
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STEREO-A Brightness Comparison
Only the STELab IPS time period is compared here
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Summary

• We follow CIR and CME structure from near the
  solar surface outward until they are observed in
  situ near Earth and at other deep-space
  spacecraft.
• Our fake brightness reconstructions as compared
  with STEREO HI-2s show some similarities
  (qualitatively).
• The WHI 3D-tomographic reconstructions using
  STELab IPS data give very good comparison with
  ground truth in situ measurements in five out
  of the six main comparisons shown here (the ACE
  level-0 data are not included in this count).

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Future Prospects

• Were in the process of further in situ
  comparisons with Wind and the twin STEREO
  spacecraft, and other deep-space spacecraft
  particularly where other interesting
  observations/measurements overlap.
• We have now devised a wealth of tools to
  understand and analyze the SMEI image data, and
  to ascertain how well the SMEI 3D reconstructions
  work of primary importance here is the
  comparison with STEREO in situ and imaging
  observations, and future STEREO 3D-reconstruction
  analyses.

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Acknowledgements and Primary Reference
Special thanks go to the Jackie Davies at the
Rutherford-Appleton Laboratory (RAL), Didcot,
England, UK, for the STEREOSECCHI HI-2 (A and
B) images used in this study. Thanks also to
the WindSWE, ACESWEPAM, and STEREOPLASTIC
teams for making their in situ data available on
the Web. - Bisi, M.M., B.V. Jackson, A.
Buffington, J.M. Clover, P.P. Hick, and M.
Tokumaru, Low-Resolution STELab IPS 3D
Reconstructions of the Whole Heliosphere Interval
and Comparison with in-Ecliptic Solar Wind
Measurements from STEREO and Wind
Instrumentation, Solar Physics, STEREO Science
Results at Solar Minimum Special Edition,
doi10.1007/s11207-009-9350-9, 2009 http//stesu
n5.stelab.nagoya-u.ac.jp/uhf_ant-e.html
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BONUS!
Post-WHI CME reconstructed with higher-resolution
3D tomographic from Solar Mass Ejection Imager
(SMEI) data
See the Jackson, B.V., M.M. Bisi, P.P. Hick, A.
Buffington, J.M. Clover, D.F. Webb, and M.
Tokumaru talk Friday at 0930h!