Solar Physics

, Volume 227, Issue 2, pp 339–353

Comparative Analyses of the CSSS Calculation in the UCSD Tomographic Solar Observations

Authors

    • Center for Astrophysics and Space SciencesUniversity of California at San Diego
  • B. V. Jackson
    • Center for Astrophysics and Space SciencesUniversity of California at San Diego
  • P. P. Hick
    • Center for Astrophysics and Space SciencesUniversity of California at San Diego
  • A. Buffington
    • Center for Astrophysics and Space SciencesUniversity of California at San Diego
  • X. P. Zhao
    • W.W. Hansen Experimental Physics LaboratoryStanford University
Article

DOI: 10.1007/s11207-005-2759-x

Cite this article as:
Dunn, T., Jackson, B.V., Hick, P.P. et al. Sol Phys (2005) 227: 339. doi:10.1007/s11207-005-2759-x

Abstract

We describe a new method to derive the interplanetary magnetic field (IMF) out to 1 AU from photospheric magnetic field measurements. The method uses photospheric magnetograms to calculate a source surface magnetic field at 15R. Specifically, we use Wilcox Solar Observatory (WSO) magnetograms as input for the Stanford Current-Sheet Source-Surface (CSSS) model. Beyond the source surface the magnetic field is convected along velocity flow lines derived by a tomographic technique developed at UCSD and applied to interplanetary scintillation (IPS) observations. We compare the results with in situ data smoothed by an 18-h running mean. Radial and tangential magnetic field amplitudes fit well for the 20 Carrington rotations studied, which are largely from the active phase of the solar cycle. We show exemplary results for Carrington rotation 1965, which includes the Bastille Day event.

Copyright information

© Springer Science + Business Media, Inc. 2005