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

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Presentation transcript:

B.V. Jackson H.-S. Yu, P.P. Hick, A. Buffington, M. Tokumaru Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA M. Tokumaru Institute for Space-Earth Environmental Research (ISEE), Nagoya University, Nagoya 464-8601, Japan A. Gonzalez-Espararza, J. Mejia-Ambriz, O. Chang SCIESMEX, Instituto de Geofisica, UNAM, Morelia, Mexico D. Odstrcil George Mason University, Fairfax, Virginia, and NASA-Goddard Spaceflight Center, USA S. Hong, J. Kim Korean Space Weather Center, National Radio Research Agency, 198-6, Jeju, 695-922 South Korea Where necessary I will add comments B. Lee, J. Yi, J. Yun SELab, 8, Nonhyeon-ro 150-gil, Gangnam-gu, Seoul, South Korea M.M Bisi RAL Space, Science & Technology Facilities Council, Rutherford Appleton Laboratory, Harwell Oxford, Didcot, Oxfordshire, OX11 0QX, England (UK) Masayoshi http://ips.ucsd.edu/

Today’s Predictive Analysis Where necessary I will add comments Masayoshi

IPS Heliospheric Analyses ISEE (STELab) DATA IPS Heliospheric Analyses 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. ISEE IPS array near Mt. Fuji ISEE IPS array systems

IPS Heliospheric Analyses ISEE (STELab) DATA IPS Heliospheric Analyses ISEE (STELab) Density inhomogenieties in the solar wind on the order of 150 km size from point radio sources produce an intensity pattern variation on the ground that travels away from the Sun with the solar wind speed. This pattern, measured and correlated between different radio sites in Japan allows a determination of the solar wind speed by translating this value to the line of sight perpendicular. The fuzz observed correlates from one radio site to another. IPS line-of-sight response ISEE IPS array systems

IPS line-of-sight response Sample outward motion over time 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. ISEE IPS This shows how the UCSD IPS time-dependent Computer Assisted Tomography (C.A.T.) analysis works. The 327 MHz IPS line of sight weighting provides a weight for each source observation on a spherical source surface below each line. As material moves outward from the Sun, it follows a very specific modeled path and expansion that is weighted differently at different times. The full mathematical treatment can be found in Jackson, B.V., et al., 2008, Adv. in Geosciences, 21, 339-360. Sample outward motion over time

Space Weather Predictions using IPS Heliospheric C.A.T. analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction.

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

Today’s Real-Time SOLIS CSSS Open-Field Predictions http://ips.ucsd.edu/index_br_nson_bt_nson.html Today’s Real-Time SOLIS CSSS Open-Field Predictions M Potentaily talk will proceed this way

Today’s Real-Time SOLIS CSSS Open-Field Correlations http://ips.ucsd.edu/index_br_nson_bt_nson.html Today’s Real-Time SOLIS CSSS Open-Field Correlations M Potentaily talk will proceed this way

IPS Get-together at UCSD UCSD IPS Workshop 18-20 December – First Announcement Bernard V. Jackson (bvjackson@ucsd.edu) J. Americo Gonzalez-Esparza (americo.glz@gmail.com) Mario M. Bisi (Mario.Bisi@stfc.ac.uk) Munetoshi Tokumaru (tokumaru@stelab.nagoya-u.ac.jp) Dear Colleagues, We will be having a small IPS-based workshop (including associated Faraday rotation prospects) held 18-20 December, 2016, in La Jolla, CA, USA, at UCSD immediately following the 2016 fall AGU meeting in San Francisco, CA, USA. This mini-workshop was decided-upon as a good time to present updated results from the Third Remote Sensing Workshop held 20-24 October, 2015 in Morelia, Michoacan, Mexico.

IPS Get-together at UCSD Tentative agenda: (1) Progress towards international WIPSS organization and collaborative efforts. (2) Single and multi-site IPS analyses and comparisons (including the determination of accurate velocity and g-level values with errors). (a) Different methods of determining single-site speeds. (b) Different methods of determining error values for IPS speeds and g-levels - which techniques work best, and why. (c) Different methods of IPS data presentation – skymaps, timeseries, etc. (d) IPS tomographic data representations of these data sets. (e) Use of these data sets with heliospheric 3D-MHD analyses. (3) Progress toward providing the simplified ASCII (txt file) IPS output (IPSCDFv1.0), the agreed-upon standard data format, from all sites; its implementation in near real time, and as an archival data set. (a) Best ways to provide IPS g-levels in near real time. (b) Provision of more complete IPS data sets for colleague access at host sites. (4) Heliospheric Faraday rotation (FR) experiment design and implementation including discussion on progress thus far achieved and/or published.

ORIGINALD ANALYSIS (White Light) Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 27-28 May 2003 CME event period ORIGINALD ANALYSIS (White Light) Full SMEI data set, 6-hour cadence, 3º x 3º lat, long SMEI proton density reconstruction for the 27-28 May 2003 halo CME sequence. Reconstructed and ACE L2 in-situ densities are compared over one Carrington rotation.

SMEI Webpages - http://smei.ucsd.edu The SMEI instrument was closed by the Air Force in September 2011, UCSD maintains the only SMEI Web pages and has upgraded them at: http://smei.ucsd.edu. SMEI high resolution tomography has been used to reconstruct a filament at 1 AU! SMEI Webpages - http://smei.ucsd.edu

Future? Cut-away and schematic Characteristics Jackson,B.V., et al., 2004, Solar Phys., 225, 177-207. All sky view to within 2º (7.5Rs) of the Sun SMEI heritage Future? Cut-away and schematic Characteristics Jackson,B.V., et al., 2010, Solar Phys., 265, 257–275.

Instrumentation Accomodation Future? PERSEUS Instrumentation Accomodation