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Coronal Faraday Rotation: Diagnostics of Current Sheets and MHD Waves

Scope of Talk: Observations of Extragalactic Radio Sources with Radio Interferometers. Very Large Array. Radio interferometer27 antennasB or A arrayObservations taken at 1465 and 1665 MHz. Advantages of Interferometric Observations of Extragalactic Radio Sources. Simultaneous measurements on a set of lines of sight (pharetra) through the coronaUse of

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Coronal Faraday Rotation: Diagnostics of Current Sheets and MHD Waves

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    1. Coronal Faraday Rotation: Diagnostics of Current Sheets and MHD Waves

    2. Scope of Talk: Observations of Extragalactic Radio Sources with Radio Interferometers

    3. Very Large Array

    4. Advantages of Interferometric Observations of Extragalactic Radio Sources Simultaneous measurements on a set of lines of sight (pharetra) through the corona Use of “constellations” of radio sources for tomographic-like analyses

    5. Plasma Contributions to the Faraday Rotation Integral

    6. New Coronal Faraday Rotation Results from the VLA Project AS764: August, 2003; 2X10 hour sessions on source 3C228 Project AS826: March-April 2005; 4X10 hour sessions (plus reference) for coronal “tomography”

    7. Project AS826

    8. Results from Project AS764: Continuous Observations of 3C228 on August 16 and 18, 2003 Measurement of RM(t) to source as a whole Measurement of “Differential Faraday Rotation”, different rotation measures along different lines of sight (A,B, and C)

    9. Faraday Rotation to 3C228 on August 16, 2003 Remarkably little differential Faraday rotation observed

    10. Modeling the Observed Rotation Measure

    11. Spatial Structure Function (no Taylor Hypothesis!)

    12. Spatial Structure Function (no Taylor Hypothesis!)

    13. Preliminary and Tentative Rotation Measure Structure Function Results August 16, 15.77-18.62 UT: DRM < 0.38 rad/m2 August 16, 20.53-23.22 UT: DRM < 4.8 rad/m2 August 18, 20 -24 UT: DRM < 0.25 rad/m2

    14. Meaning of Result in Terms of Coronal Plasma Parameters

    15. Quantitative Significance of Observed RM Structure Functions

    16. How Can Faraday Rotation Observations Probe the Overall Structure of the Coronal Plasma? (AS826)

    17. Global RM Models: How well can synoptic coronal models account for FR Measurements?

    18. AS826 Preliminary Results

    24. AS826: Use of Synoptic Model for Corona

    25. Estimating the distant coronal plasma from measurements at ~3 R

    26. How radio line of sight probes the corona

    27. Observed and Model RM Comparison-AS826

    28. Observed and Model RM Comparison

    29. Observed and Model RM Comparison

    30. Conclusions Simple synoptic models of the corona roughly reproduce “Pharetrae” of Faraday Rotation measurements, but large residuals. Measurements consistent with coronal field of 30-80mG at r=6R. (Paetzold 1987) Rotation measure changes substantially on timescales of a few hours; too slow to be turbulence. Thus “Mesoscale Plasma Structures”. Smaller, faster fluctuations attributable to waves seen in spacecraft beacon data. Spatial variations in RM (differential Faraday Rotation) are small; constraints on coronal turbulence are reasonable but not decisive

    31. Future Developments EVLA (Expanded VLA): Enormous increase in sensitivity of the VLA, in progress. But only if feed design prevents system temperature increase due to Sun. VLA at 5 GHz: Could make measurements closer to the Sun, observations have more impact.

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