Determination of the North-South Heliospheric Magnetic Field from Inner-Corona Closed-Loop Propagation B.V. Jackson Center for Astrophysics and Space Sciences,

Slides:

Advertisements

Similar presentations

K. Fujiki, H. Ito, M. Tokumaru Solar-Terrestrial Environment Laboratory (STELab), Nagoya University. SOLAR WIND FORECAST BY USING INTERPLANETARY SCINTILLATION.

Advertisements

H.-S. Yu Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA 3D-MHD Models Driven by IPS

Global Properties of Heliospheric Disturbances Observed by Interplanetary Scintillation M. Tokumaru, M. Kojima, K. Fujiki, and M. Yamashita (Solar-Terrestrial.

“Insights” on Coronal Hole Magnetic Fields From a High-Order PFSS Model D.J. Bercik and J.G. Luhmann Space Sciences Lab, UC Berkeley 1 FEW 2011, Aug 24.

Synoptic maps and applications Yan Li Space Sciences Laboratory University of California, Berkeley, CA HMI team meeting, Jan 27, 2005, Stanford.

Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.

February 26, 2007 KIPAC Workshop on Magnetism Modeling/Inferring Coronal And Heliospheric Field From Photospheric Magnetic Field Yang Liu – Stanford University.

Absence of a Long Lasting Southward Displacement of the HCS Near the Minimum Preceding Solar Cycle 24 X. P. Zhao, J. T. Hoeksema and P. H. Scherrer Stanford.

UCB MURI Team Introduction An overview of ongoing work to understand a well observed, eruptive active region, along with closely related studies…..

Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.

What coronal parameters determine solar wind speed? M. Kojima, M. Tokumaru, K. Fujiki, H. Itoh and T. Murakami Solar-Terrestrial Environment Laboratory,

CASS/UCSD SALE 2014 An Account of Space Weather at Comet 67P/C-G H.-S. Yu, P.P. Hick, A. Buffington University of California at San Diego, LaJolla, California,

1 C. “Nick” Arge Space Vehicles Directorate/Air Force Research Laboratory SHINE Workshop Aug. 2, 2007 Comparing the Observed and Modeled Global Heliospheric.

CASS/UCSD AFOSR 2014 IPS 3D Velocity and Density Analysis B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San Diego,

CASS/UCSD KSSS D Analysis of Remote-sensed Heliospheric Data B.V. Jackson, H.-S. Yu, P.P. Hick, A. Buffington University of California at San Diego,

Topical Issue (TI) in Solar Physics – Used as a Proceedings for this Workshop with a Much Broader Capture of Important Radio-Heliophysics Papers… IPS Workshop.

Solar System Physics Group Heliospheric physics with LOFAR Andy Breen, Richard Fallows Solar System Physics Group Aberystwyth University Mario Bisi Center.

Comparison of the 3D MHD Solar Wind Model Results with ACE Data 2007 SHINE Student Day Whistler, B. C., Canada C. O. Lee*, J. G. Luhmann, D. Odstrcil,

Upgrade of STEL Multi-Station Interplanetary Scintillation System and Recent Observations of the Solar Wind Munetoshi Tokumaru, Masayoshi Kojima, Ken ’

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San Diego,

The Solar Wind.

Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Heliosphere: The Solar Wind March 01, 2012.

CASS/UCSD - Jeju 2015 A Jets in the Heliosphere: A Solar Wind Component B.V. Jackson, H.-S. Yu, P.P. Hick, and A. Buffington, Center for Astrophysics and.

Faraday Rotation: Unique Measurements of Magnetic Fields in the Outer Corona Justin C. Kasper (UM), Ofer Cohen (SAO), Steven Spangler (Iowa), Gaetan Le.

Conclusions Using the Diffusive Equilibrium Mapping Technique we have connected a starting point of a field line on the photosphere with its final location.

1 University of California, San Diego, U.S.A., 2 NASA - Goddard Space Flight Center, U.S.A., 3 George Mason University, U.S.A., 4 Naval Research Laboratory,

Measurements of White-Light Images of Cometary Plasma as a Proxy for Solar Wind Speed J.M. Clover, M.M. Bisi, A. Buffington, B.V. Jackson, P.P. Hick Center.

3 rd RSIH&SWA Workshop – Morelia, Mexico – October 2015 Agenda M.M. Bisi (1). (1) RAL Space, Science and Technology Facilities.

3 rd RSIH&SWA Workshop – Morelia, Mexico – 24 October 2015 New Opportunities for IPS - A Personal Perspective M.M. Bisi (1). (1)

CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks B.V. Jackson, P.P. Hick, A. Buffington, M.M. Bisi, J.M. Clover, S. Hamilton Center.

1 Center for Astrophysics and Space Sciences, University of California, San Diego 9500 Gilman Drive #0424, La Jolla, CA , U.S.A

1 Center for Astrophysics and Space Sciences, University of California, San Diego 9500 Gilman Drive #0424, La Jolla, CA , U.S.A

1 Center for Astrophysics and Space Sciences, University of California, San Diego 9500 Gilman Drive #0424, La Jolla, CA , U.S.A

1 Center for Astrophysics and Space Sciences, University of California, San Diego 9500 Gilman Drive #0424, La Jolla, CA , U.S.A

IPS 3D reconstructions and their comparison with STEREO and Wind spacecraft Mario M. Bisi 1 Bernard V. Jackson 1, John M. Clover 1,

1 Center for Astrophysics and Space Sciences, University of California, San Diego 9500 Gilman Drive #0424, La Jolla, CA , U.S.A

Center for Astrophysics and Space Sciences, University of California, San Diego 9500 Gilman Drive #0424, La Jolla, CA , U.S.A

1 Center for Astrophysics and Space Sciences, University of California, San Diego 9500 Gilman Drive #0424, La Jolla, CA , U.S.A

CASS/UCSD Dusan_CCMC_2013 Heliospheric Solar Wind Forecasting Using IPS Slides For A Possible CCMC Presentation 2013 Introduction:

1 Pruning of Ensemble CME modeling using Interplanetary Scintillation and Heliospheric Imager Observations A. Taktakishvili, M. L. Mays, L. Rastaetter,

1 CASS, University of California, San Diego, U.S.A. ; 2 STFC Rutherford Appleton Laboratory, UK; 3 George Mason University, U.S.A.; 4 NASA/GSFC,

A 3D-MHD Model Interface Using Interplanetary Scintillation (IPS) Observations B.V. Jackson 1, H.-S. Yu 1, P.P. Hick 1, A. Buffington 1, D. Odstrcil 2,

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.

CASS/UCSD RSW Space Weather Forecasting from IPS Data Sets M. Tokumaru Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya ,

Long-term measurements of the Sun’s poles show that reversal of the dominant magnetic polarity generally occurs within a year of solar maximum. Current.

CASS/UCSD SWG SMEI observations and comparison with STEREO SMEI direct observations and 3D-reconstruction measurements and their comparison with.

H.-S. Yu 1, B.V. Jackson 1, P.P. Hick 1, A. Buffington 1, M. M. Bisi 2, D. Odstrcil 3,4, M. Tokumaru 5 1 CASS, UCSD, USA ; 2 STFC RALab, Harwell Oxford,

Using World Interplanetary Scintillation Systems

B.V. Jackson H.-S. Yu, P.P. Hick, A. Buffington,

B.V. Jackson, H.-S. Yu, P.P. Hick, and A. Buffington,

Driving 3D-MHD codes Using the UCSD Tomography

Nicholeen Viall NASA/GSFC

Observations of Heliospheric Faraday Rotation

The Worldwide Interplanetary Scintillation (IPS) Stations (WIPSS) Network Mario M. Bisi [1], J. Americo Gonzalez-Esparza[2][3][4],

H.-S. Yu1, B.V. Jackson1, P.P. Hick1,

B.V. Jackson, and P.P. Hick, A. Buffington, M.M. Bisi, J.M. Clover

The Dynamic Character of the Polar Solar Wind

Xuepu Zhao Oct. 19, 2011 The Base of the Heliosphere: The Outer (Inner) Boundary Conditions of Coronal (Heliospheric) models.

2014SWW - S9 3D Reconstruction of IPS Remote-sensing Data: Global Solar Wind Boundaries for Driving 3D-MHD Models Hsiu-Shan Yu1, B.V. Jackson1, P.P. Hick1,

ST23-D2-PM2-P-013 The UCSD Kinematic Global Solar Wind Boundary for use in ENLIL 3D-MHD Forecasting Bernard JACKSON1#+, Hsiu-Shan YU1, Paul HICK1, Andrew.

IPS Heliospheric Analyses (STELab)

Bernard V. Jackson1, Hsiu-Shan Yu1, P

Exploration of Solar Magnetic Fields from Propagating GONG Magnetograms Using the CSSS Model and UCSD Time-Dependent Tomography H.-S. Yu1, B. V. Jackson1,

B.V. Jackson H.-S. Yu, P.P. Hick, A. Buffington, M. Tokumaru

Bernard V. Jackson, P. Paul Hick, Andrew Buffington, John M. Clover

D. Odstrcil1,2, V.J. Pizzo2, C.N. Arge3, B.V.Jackson4, P.P. Hick4

B.V. Jackson H.-S. Yu, P.P. Hick, A. Buffington, M. Tokumaru

The Worldwide Interplanetary Scintillation (IPS) Stations (WIPSS) Network: Initial Results from the October 2016 Space-Weather Campaign © 2017 RAL Space.

Investigation of Heliospheric Faraday Rotation Due to a Coronal Mass Ejection (CME) Using the LOw Frequency ARray (LOFAR) and Space-Based Imaging Techniques.

ESS 261 Topics in magnetospheric physics Space weather forecast models ____ the prediction of solar wind speed April 23, 2008.

Presentation transcript:

Determination of the North-South Heliospheric Magnetic Field from Inner-Corona Closed-Loop Propagation B.V. Jackson 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 M.M. Bisi RAL Space, Science & Technology Facilities Council, Rutherford Appleton Laboratory, Harwell Oxford, Didcot, Oxfordshire, OX11 0QX, England (UK) M. Tokumaru Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan Where necessary I will add comments J. Kim, S. Hong Korean Space Weather Center, National Radio Research Agency, 198-6, Jeju, 695-922 South Korea B. Lee, J. Yi, J Yun SELab, 8, Nonhyeon-ro 150-gil, Gangnam-gu, Seoul, South Korea Masayoshi http://smei.ucsd.edu/ http://ips.ucsd.edu/

Introduction: IPS Magnetic Field forward modeling closed-loop analyses from Current Sheet Source Surface (CSSS) modeling Closed-loop component forward-modeling of Bn can show a low-resolution component in solar wind data Current studies so far, implications My talk will proceed this way

Interplanetary Scintillation (IPS) Analysis 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.

Current Prediction Analyses Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115. http://ips.ucsd.edu/ Current Prediction Analyses UCSD IPS analysis UCSD Web pages The UCSD forecast website. Web Analysis Runs Automatically Using Linux on a P.C.

UCSD Archival IPS Analysis of V and D at WIND over Carrington rotation 2056 (April 27 – May 25, 2007) velocity density

Magnetic Field

Magnetic Field Extrapolation (Zhao, X. P. and Hoeksema, J. T., 1995, J. Geophys. Res., 100 (A1), 19.) http://ips.ucsd.edu/ Magnetic Field Extrapolation Dunn et al., 2005, Solar Physics 227: 339–353. In a technique worked out by Zhao, X. P. and Hoeksema, J. T., 1995, J. Geophys. Res., 100 (A1), 19, we are able to project outward magnetic field from the solar surface. This works globally using archival data or in forecast. The potential field model provides a measurement of radial field at the source surface. This is projected outward using the UCSD solar wind model to provide a radial and tangential field anywhere within the 3D volume. Inner region: the CSSS model calculates the magnetic field using photospheric 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. Jackson, B.V., et al., 2011, Adv. in Geosciences, 30, 93-115

15 Rs source surface Br field component sample (Zhao, X. P. and Hoeksema, J. T., 1995, J. Geophys. Res., 100 (A1), 19.) CSSS model 15 Rs source surface Br field component sample Dunn et al., 2005, Solar Physics 227: 339–353. Exclusively NSO SOLIS DATA

“R” “T” “N”

Extrapolated Br field component for CR 2056 CSSS model Extrapolated Br field component for CR 2056 Extrapolated Bt field component for CR 2056

“R” “T” “N” However, I have often wondered where the Bz in-situ field comes from. The Parker spiral analysis does not indicate how a normal field (north-south) can occur, and yet the field exists.

What is really wanted is Bn  Bz

1.3Rs below cusp surface Bn field component sample (Jackson, B.V., et al., 2015, ApJL, 803:L1. 1- 5, doi:10.1088/2041-8205/803/1/L1.) CSSS model 1.3Rs below cusp surface Bn field component sample

Extrapolated Bn field component for CR 2056 (Jackson, B.V., et al., 2015, ApJL, 803:L1. 1- 5, doi:10.1088/2041-8205/803/1/L1.) CSSS model Extrapolated Bn field component for CR 2056 About 1/50th of the static flux r-1.34 fall-off

Things to try to determine a more Study Underway Things to try to determine a more consistent closed loop and Bn correlation: 1) Will another model of the closed flux change the result? 2) How does the correlation and amount of closed flux released change from one Carrington rotation to another? 3) How does the location of the flux release surface change the result? 4) Do different magnetogram inputs provide a different result?

Structure at 1. 3Rs flux release surface sample field Structure at 1.3Rs flux release surface sample field components from CSSS and PFSS models. PFSS Br PFSS Bt PFSS Bn CSSS Br CSSS Bt CSSS Bn

Variation with Solar Cycle

1.3Rs below cusp surface Br field component sample (Jackson, B.V., et al., 2015, ApJL, 803:L1. 1- 5, doi:10.1088/2041-8205/803/1/L1.) CSSS model 1.3Rs below cusp surface Br field component sample

Extrapolated Br field component for CR 2056 (Jackson, B.V., et al., 2015, ApJL, 803:L1. 1- 5, doi:10.1088/2041-8205/803/1/L1.) CSSS model Extrapolated Br field component for CR 2056 1/50th of the static flux r-1.34 fall-off

Br ten-year correlation summary plot Work in progress

Br ten-year slope summary plot Work in progress

We suggest that at least part of the Bn component comes from closed fields that escape from near the solar surface – perhaps through some non-static process.

1.3 Rs “traced” near cusp surface Bn field component sample CSSS model 1.3 Rs “traced” near cusp surface Bn field component sample Work in progress

Summary: IPS Magnetic Field forward modeling closed-loop analyses from Current Sheet Source Surface (CSSS) modeling can be forward modeled to show all three components of magnetic field measured in-situ. The results so far are low resolution, and while all three “closed” components give a dominance of positive correlations, the correlations from one to the next Carrington rotation are not always positive. The results show that these components are more dominant when there is a larger amount of solar activity. The implication is that probably some remnant of the closed fields escape from the near solar surface to permeate the solar wind. My talk will proceed this way

1.3Rs below cusp surface Bt field component sample (Jackson, B.V., et al., 2015, ApJL, 803:L1. 1- 5, doi:10.1088/2041-8205/803/1/L1.) CSSS model 1.3Rs below cusp surface Bt field component sample

Extrapolated Bt field component for CR 2056 (Jackson, B.V., et al., 2015, ApJL, 803:L1. 1- 5, doi:10.1088/2041-8205/803/1/L1.) CSSS model Extrapolated Bt field component for CR 2056 1/50th of the static flux r-1.34 fall-off

Bt ten-year correlation summary plot Work in progress

Bt ten-year slope summary plot Work in progress

Bn ten-year correlation summary plot Work in progress

Bn ten-year slope summary plot Work in progress

Structure at and below the cusp surface Bn field component sample.