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Coronal Faraday Rotation: Diagnostics of Current Sheets and MHD Waves. Steven R. Spangler, Laura D. Ingleby, Laura G. Spitler, Catherine A. Whiting. Scope of Talk: Observations of Extragalactic Radio Sources with Radio Interferometers. Very Large Array. Radio interferometer 27 antennas - PowerPoint PPT Presentation
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Coronal Faraday Rotation: Diagnostics of Current Sheets and MHD Waves
Steven R. Spangler, Laura D. Ingleby, Laura G. Spitler, Catherine A. Whiting
Scope of Talk: Observations of Extragalactic Radio Sources with Radio Interferometers
Very Large Array
• Radio interferometer• 27 antennas• B or A array• Observations 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 corona
• Use of “constellations” of radio sources for tomographic-like analyses
Plasma Contributions to the Faraday Rotation Integral
We need enough observations to sort out various contributions to coronal density and magnetic field
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”
Project AS826
o Observations:•March 12
•March 19
•March 28
•April 1
•May 29 (reference)
o 19 sources, 20 lines of sight
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)
Faraday Rotation to 3C228 on August 16, 2003
Remarkably little differential Faraday rotation observed
Modeling the Observed Rotation Measure
Spatial Structure Function (no Taylor Hypothesis!)
Spatial Structure Function (no Taylor Hypothesis!)
Diff. RM feature
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
Meaning of Result in Terms of Coronal Plasma Parameters
From Minter and Spangler (1996), magnetic field fluctuations only
Turbulence properties
Quantitative Significance of Observed RM Structure Functions
August 16, 6.2R August 18, 5.2R
l=0.1R
L=1.0R
e=0.5
e=1.0
How Can Faraday Rotation Observations Probe the Overall Structure of the Coronal
Plasma? (AS826)
Global RM Models: How well can synoptic coronal models account for FR Measurements?
Mancuso and Spangler 2000
Residuals of ~ 2-3 rad/sq-m
AS826 Preliminary ResultsSource RM Average Error
2323-033 61.068 0.9976
2325-049 6.952 0.7295
2326-020 -2.418 0.9832
2328-049 -4.163 0.65297
2331-015 -6.087 2.564
2335-015 -13.671 0.305
2337-025 -12.458 0.4514
2338-042 -4.993 0.2619
2351-012 -27.35
0.693
2352-016 -24.175 1.428
2357-024 3.145 0.202
0006-001 2.255 0.207
0023+045 5.18 0.125
0029+052 -2.515 0.196
0030+058 0.582 0.685
0034+013 1.92 0.58
0039+033 2.272 1.27
0039+033 -0.905 0.79
0041+070 -0.371 0.613
0046+067 -14.067 1.509
2RM
AS826: Use of Synoptic Model for Corona
These measurements of magnetic field and density at ~ 3R can be used to estimate B and n at greater distances probed by Faraday Rotation
Estimating the distant coronal plasma from measurements at ~3 R
An and AB are arbitrary adjustment factors
How radio line of sight probes the corona
Observed and Model RM Comparison-AS826
Observed and Model RM Comparison
Observed and Model RM Comparison
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
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.