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Radio
observations still the only means for reliably
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measuring
coronal magnetic field strengths anywhere on
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the solar disk
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Measures
temperatures on surface of constant field
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strength
– directly see regions of strong heating
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Because
emission is optically thick in regions of strong
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field,
we get 3D information on fields
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Relatively
insensitive to density, therefore complements
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EUV/soft
X-ray observations which are dominated by
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density
contrast
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Important
role in testing techniques for extrapolating
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surface
fields into corona
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