Introduction of the CSSS magnetic field calculation into the UCSD tomographic solar wind model

Details Introduction of the CSSS magnetic field calculation into the UCSD tomographic solar wind model Introduction of the CSSS magnetic field calculation into the UCSD tomographic solar wind model

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spie.4853..504d&link_type=abstract

Innovative Telescopes and Instrumentation for Solar Astrophysics. Edited by Stephen L. Keil, Sergey V. Avakyan . Proceedings o

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Tomographic techniques developed at UCSD over the last few years incorporate a kinematic model of the solar wind to determine and forecast the large-scale three-dimensional extents of velocity and density using interplanetary scintillation (IPS) observations or Thomson scattering brightness data. In this paper, we introduce magnetic field calculations from the Stanford Current-Sheet Source Surface (CSSS) model into our kinematic model. The CSSS model is used to extrapolate the photospheric magnetic field to a source surface at 15 solar radii (Rs). The UCSD kinematic model convects magnetic field from 15 Rs out to and beyond Earth. We compare the results with in situ data near Earth. The spatial relationship between the heliospheric current sheet and coronal mass ejections (CMEs) is shown in remote views of the inner heliosphere

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