Experimental constraints on pulsed and steady state models of the solar wind near the Sun

Details Experimental constraints on pulsed and steady state models of the solar wind near the Sun Experimental constraints on pulsed and steady state models of the solar wind near the Sun

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997jgr...10226905f&link_type=abstract

Journal of Geophysical Research, Volume 102, Issue A12, p. 26905-26918

Astronomy and Astrophysics

Astrophysics

31

Interplanetary Physics: Solar Wind Plasma, Interplanetary Physics: Sources Of The Solar Wind, Solar Physics, Astrophysics, And Astronomy: Corona, And Astronomy: Coronal Holes

Scientific paper

Ulysses observations of the high-latitude solar wind were combined with Spartan 201 observations of the corona to investigate the nature and extent of uncertainties in our knowledge of solar wind structure near the Sun. In addition to uncertainties stemming from the propagation of errors in density profiles inferred from coronagraph observations [see, e.g., Lallement et al., 1986], an assessment of the consequences of choosing different analysis assumptions reveals very large, fundamental uncertainties in our knowledge of even the basics of coronal structure near the Sun. In the spirit of demonstrating the nature and extent of these uncertainties we develop just one of a generic class of explicitly time-dependent and filamentary models of the corona that is consistent with the Ulysses and Spartan 201 data. This model provides a natural explanation for the radial profiles of both the axial ratios and apparent radial speeds of density irregularities measured at radial distances less than 10RS using the interplanetary scintillation technique.

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