Abstract
We have developed a computer-assisted tomography (CAT) technique that iteratively modifies a kinematic solar wind model to least-squares fit heliospheric remote sensing observations (interplanetary scintillation and Thomson-scattering observations). These remote sensing data cover a large range of solar elongations, and access high-latitude regions over the solar poles. The technique can be applied to a time-independent solar wind model, assuming strict co-rotation, or, when sufficient remote sensing observations are available, to a time-dependent model. For the time-dependent case the technique depends primarily on outward motion of structures in the solar wind to provide the perspective views required for a tomographic reconstruction. We show results of corotating tomographic reconstructions primarily using IPS velocity observations from the Solar-Terrestrial Environment Laboratory (STELab, Nagoya, Japan), and include comparisons with in situ velocity data out of the ecliptic (Ulysses) and in the ecliptic (ACE).
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References
Asai, K., Kojima, M., Tokumaru, M., Yokobe, A., Jackson, B. V., Hick, P. L., and Manoharan, P. K.: 1998, `Heliospheric Tomography Using Interplanetary Scintillation Observations, 3. Correlation Between Speed and Electron Density Fluctuations in the Solar Wind’, J. Geophys. Res. 103 (A2), 1991–2001.
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© 2001 Springer Science+Business Media Dordrecht
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Hick, P.P., Jackson, B.V. (2001). Three-Dimensional Solar Wind Modeling Using Remote-Sensing Data. In: Marsden, R.G. (eds) The 3-D Heliosphere at Solar Maximum. Springer, Dordrecht. https://doi.org/10.1007/978-94-017-3230-7_6
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DOI: https://doi.org/10.1007/978-94-017-3230-7_6
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-481-5723-5
Online ISBN: 978-94-017-3230-7
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