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The Ability of Radio Heliospheric Remote Sensing Observations to Provide Global Solar Wind Parameters. Bernard V. Jackson, P. Paul Hick, Andrew Buffington, Hsiu-Shan Yu, Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA Mario M. Bisi

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slide1

The Ability of Radio Heliospheric Remote Sensing Observations to Provide Global Solar Wind Parameters

Bernard V. Jackson, P. Paul Hick,

Andrew Buffington, Hsiu-Shan Yu,

Center for Astrophysics and Space Sciences,

University of California at San Diego, LaJolla, CA, USA

Mario M. Bisi

Institute of Mathematics and Physics, Aberystwyth University, Penglais Campus, Aberystwyth, Wales, UK

Richard A. Fallows

ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, Netherlands

http://ips.ucsd.edu/ http://smei.ucsd.edu/

Masayoshi

slide2

Introduction:

The data: Interplanetary Scintillation (IPS)

STELab, Ooty, EISCAT

3D density and velocity reconstructions from IPS

Recent programming enhancements and

their use in forecasting

The Future – MEXART, Possible Faraday rotation

observations

ips heliospheric analyses stelab
IPS Heliospheric Analyses (STELab)

DATA

IPS line-of-sight response

STELab IPS array near Mt. Fuji

STELab IPS array systems

current stelab toyokawa ips system
Current STELab Toyokawa IPS System

New STELab IPS array in Toyokawa (3,432 m2 array now operates well – year-round operation began in 2011)

other current operating ips radio systems
Other Current Operating IPS Radio Systems

The Ootacamund (Ooty), India off-axis parabolic cylinder 530 m long and 30 m wide (15,900 m2) operating at a nominal frequency of 326.5 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).

other current operating ips radio systems1
Other Current Operating IPS Radio Systems

Above: The European Incoherent SCATter radar (EISCAT) and EISCAT Svalbard Radar (ESR) radio telescopes from left-to-right: Tromsø, Norway (M.M. Bisi, October 2003);

Kiruna, Sweden (M.M. Bisi, May 2003); Sodankylä, Finland (http://www.eiscat.com/sodan.html); and the ESR 42m in the foreground and steerable 32m in the background (M.M. Bisi, May 2005).

Left: The Multi-Element Radio-Linked Interferometer Network (MERLIN) MkIa (Lovell) radio telescope at Jodrell Bank (near Manchester, England); and

Right: The MERLIN MkII radio telescope also at Jodrell Bank (M.M. Bisi, May 2004).

The Ootacamund (Ooty), India off-axis parabolic cylinder 530 m long and 30 m wide (15,900 m2) operating at a nominal frequency of 326.5 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).

world wide ips observation network
World-Wide IPS observation network

Pushchino103MHz

70,000㎡

STEL Multi-Station 327MHz

2000 ㎡×3, 3500 ㎡

MEXART

140MHz、10,000㎡

IPS

UK/EISCAT

LOFAR)

Russia

Korea

Japan

India

Mexico

MWA

80-300MHz

Ooty 327MHz、16,000㎡

US-Australia

slide8

IPS line-of-sight response

Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, 339-360.

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

Sample outward motion over time

slide9

Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, 339

Relative Weighting

Outward Radial Motion

slide10

IPS line-of-sight response

Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, 339-360.

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

14 July 2000

13 July 2000

ips c a t analysis
IPS C.A.T. Analysis

Jackson, B.V., et al., 2002, Solar Wind 10, 31

Bastille Day Event 14 July 2000

ips c a t analysis1
IPS C.A.T. Analysis

Jackson, B.V., et al., 2002, Solar Wind 10, 31

Bastille Day Event 14 July 2000

ips c a t analysis2
IPS C.A.T. Analysis

Jackson, B.V., et al., 2002, Solar Wind 10, 31

Bastille Day Event 14 July 2000

ips c a t analysis3
IPS C.A.T. Analysis

Jackson, B.V., et al., 2002, Solar Wind 10, 31

Bastille Day Event 14 July 2000

IPS Density Meridional Cut

IPS Density LOS X-ing Meridional Cut

slide15

Zhao, X. P. and Hoeksema, J. T., 1995, J. Geophys. Res., 100 (A1), 19.

http://ips.ucsd.edu/

Magnetic Field Extrapolation

  • Inner region: the CSSS model calculates the magnetic field usingphotospheric measurements and a horizontal current model.

2. Middle region: the CSSS model opens the field lines. In the outer region.

3. Outer region: the UCSD tomography convects the magnetic field along velocity flow lines.

Dunn et al., 2005, Solar Physics 227: 339–353.

Jackson, B.V., et al., 2012, Adv. in Geosciences, 30, 93-115.

ips c a t analysis4
IPS C.A.T. Analysis

Dunn, T.J., et al., 2005, Solar Phys., 227, 339

Potential field modeling added

IPS Density Remote View

slide17

Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256.

IPS line-of-sight response

Jackson, B.V., et al., 2010, Adv. in Geosciences, 21, 339-360.

Jackson, B.V., et al., 2012,Solar Phys. published on-line.

Heliospheric C.A.T. Analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction.

Innovation

STELab IPS

*

13 July 2000

Inclusion of in-situ measurements into the 3D-reconstructions

heliospheric 3d reconstructions
Heliospheric 3D-reconstructions

Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256.

Innovation

Innovation

Inclusion of in-situ measurements into the 3D-reconstructions

Jackson, B.V., et al., 2008, Adv. in Geosciences, (in press).

heliospheric 3d reconstructions1
Heliospheric 3D-reconstructions

Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256.

Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115.

Forecast

Jackson, B.V., et al., 2012,Solar Phys. published on-line.

Density

Forecast

Forecast

Inclusion of in-situ measurements into the 3D-reconstructions

Forecasts work better if the values match up to the present.

Velocity

Forecast

heliospheric 3d reconstructions2
Heliospheric 3D-reconstructions

Jackson, B.V., et al., 2010,Solar Phys., 265, 245-256.

Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115.

Forecast

Jackson, B.V., et al., 2012,Solar Phys. published on-line.

Density

Density

Forecast

Inclusion of in-situ measurements into the 3D-reconstructions

Forecasts work better if the values match up to the present.

Velocity

Velocity

Forecast

slide21

Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115.

http://ips.ucsd.edu/

UCSD Web pages

UCSD IPS forecasts

Web Analysis Runs Automatically Using Linux on a P.C.

slide22

http://ips.ucsd.edu/

Skymap view

UCSD IPS forecast

Web analysis runs automatically using Linux on a P.C.

slide23

Today’s Analysis

http://ips.ucsd.edu/

Density overview

Web Analysis Runs Automatically Using Linux on a P.C.

slide24

http://ips.ucsd.edu/

Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115.

UCSD Web pages

UCSD IPS forecasts

Aftcast

Density

CCMC real-time

Aftcast

Velocity

2012 August 14 23 UT

Web Analysis Runs Automatically Using Linux on a P.C.

recent forecast
Recent Forecast

http://ips.ucsd.edu/

CME arrival on 2012/11/30 4-6 UT increase by ~8 Np/cc

Web Analysis Runs Automatically Using Linux on a P.C.

recent forecast1
Recent Forecast

http://ips.ucsd.edu/

CME arrival on 2012/11/30 4-6 UT increase by ~8 Np/cc

Web Analysis Runs Automatically Using Linux on a P.C.

slide27

Other and Potential Future IPS 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)

(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.)

slide28

Oberoi and Lonsdale, 2012, Radio Science, 47, RS0K08, doi:10.1029/2012RS004992.

Faraday rotation signals at low frequency

‗‗Φ = λ2 ∫ neB•ds

From Oberoi and Lonsdale

slide29

Future

Jackson, B.V., et al., 2008,URAS Workshop

‗‗Φ = λ2 ∫ neB•ds

Jensen, E.A., et al., 2010,Solar Phys., 265, 31

Faraday rotation tomography

Background Field, 3D UCSD Density

Background Field, 3D UCSD Density, Mulligan “Can”

slide30

Summary:

The Future is here:

  • Forecasts with the IPS data (this has worked with STELab data for about 12 years).
  • Forecasts in real-time work better now with the inclusion of in-situ data (has been available since spring, 2011) These new innovations and the inclusion of other world IPS data sets make the technique a competitive way to measure velocities and densities.
  • FR inversion to obtain vector fields may work, but needs to be incorporated with a robust method of determining density to back out accurate vector magnetic fields remotely.