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

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CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters B.V. Jackson Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA Masayoshi The Ability of Radio Heliospheric Remote Sensing Observations to Provide Global Solar Wind Parameters ftp://cass185.ucsd.edu/Presentations/2013_jeju

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters More Details IPS (three site- one site)

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters IPS Radio Systems The Ootacamund (Ooty), India off-axis parabolic cylinder 530 m long and 30 m wide (15,900 m 2 ) operating at a nominal frequency of MHz. New STELab IPS array in Toyokawa (3,432 m 2 array now operates well – year-round operation began in 2011)

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters A model of the power spectra of density fluctuations To calculate solar wind velocities using a single IPS station, we use a theoretical power spectrum: an integration of scattering layers along the line of sight (z). The spectrum depends on: λ, ε, v, Θ, α (isotropic medium). Frequency of intensity fluctuations Diffractive function (Fresnel function) Visibility function of the source Heliocentric distance at the region of IPS (point P) Wave number of solar wind irregularities q x ² + q y ² =q² Turbulence spectrum follows a potential law α ≈ 3.5 ± 0.5 Solar wind velocity Example of the model (log-log): MEXART and STEL observing frequencies. Fresnel knee Mejia-Ambriz, J., et al., 2013, AGU 2013 Presentation, May, Cancoon, Mexico.

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters Comparison between Spectrum Fitting and Cross Correlation Methods Spectrum Fitting Method (Single-station meas.) Speed V 1st. =459km/s Axial Ratio=1.07 Spectral Index=3.8 3C /9/3 Cross Correlation Method (3-station meas.) Speed V 3st. = 457±13 km/s from IPS obs. for 3C273 in 2012 V3st. (km/s) V1st. (km/s) Correlation ~0.47 V 1st /V 3st =1.04±0.24 (Courtesy of M. Tokumaru) Tokumaru, M., et al., 2013, AOGS 2013 Presentation, June, Brisbane, Australia.

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters The Marquardt Method 1) Inverse Hessian Method –A * x m = b –A * x i = -Grad(chiSq) + b –x m – x i = A -1 * (-Grad(chiSq) ) 2) Gradient Descent Method –dx = C * Grad(chiSq)

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters STEL: Single Site: Diff: AlphaARElong.theta STELSSDiff

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters AlphaARElong.theta STELSSDiff

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters AlphaARElong.theta STELSSDiff

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters v0 = 600

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters V0=

CASS/UCSD IPS 2013 Remote Sensing Solar Wind Parameters