Physics – Plasma Physics
Scientific paper
Nov 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..dppbp1019s&link_type=abstract
American Physical Society, 46th Annual Meeting of the Division of Plasma Physics, 15-19 November, 2004, Savannah, GA. MEETING I
Physics
Plasma Physics
Scientific paper
Radioastronomical propagation measurements of the solar wind yield information on density fluctuations in plasma turbulence at heliocentric distances of 0.05 - 0.20 astronomical units ( ˜ 10 - 40 solar radii). A limitation of radio scintillation measurements is that they are proportional to path integrals along the line of sight, and thus average the properties of low and high density plasma. To correct for this, magnetohydrodynamic models of the solar wind were computed for times of two radioastronomical observing sessions. A comparison of the radioastronomical observations and the models yields the parameter m ≡ ɛ^2/ [(1+ɛ^2)l_0^2/3], where ɛ is the fractional variation of plasma density, and l0 is the outer scale of the turbulence, in units of the solar radius. Our analysis yields values of m in the range 3.0 × 10-3 - 1.0 × 10-2. These values are in excellent agreement with previous estimates based on analytic models of the solar wind plasma. For l0 ≃ 1, 0.05 ≤ ɛ ≤ 0.10, which is very similar to the values measured directly at 1 astronomical unit.
Ingleby Laura
Odstrcil Dusan
Spangler Steven
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