Possibility for Coronal Magnetic Field Measurements by EUV and X-ray Spectroscopy Sophie Canton (Charge exchange) Matt Carpenter (Algorithms,CX) Jaan Lepson (EUV spectra) Henry Silva (SMM/Yohkoh data) Peter Beiersdorfer Solar Lunch SSL, 5/19/06 Your LDRD Representative Graphic Here (Fit in this rectangle, no caption)
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Possibility for Coronal Magnetic Field Measurements by EUV and X-ray Spectroscopy Sophie Canton (Charge exchange) Matt Carpenter (Algorithms,CX) Jaan Lepson.
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Possibility for Coronal Magnetic Field Measurements by EUV and X-ray Spectroscopy
Possibility for Coronal Magnetic Field Measurements by EUV and X-ray Spectroscopy
Sophie Canton (Charge exchange)Matt Carpenter (Algorithms,CX)Jaan Lepson (EUV spectra)Henry Silva (SMM/Yohkoh data)
Sophie Canton (Charge exchange)Matt Carpenter (Algorithms,CX)Jaan Lepson (EUV spectra)Henry Silva (SMM/Yohkoh data)
Peter BeiersdorferPeter Beiersdorfer
Solar LunchSSL, 5/19/06
Your LDRDRepresentativeGraphic Here(Fit in thisrectangle, nocaption)
The extreme ultraviolet is extremely rich in lines
The solar emission in the 25 – 170Å region has similar problems and more
There are few observations in this spectral band
The data from the 1970's represents the reference data that are still being used in emission models
We have been making laboratory measurements to build a catalogue of the lines in the EUV
Discovery of an X-ray line diagnostic of the magnetic field
Explanation of the magnetic-field sensitivity
Predicted magnetic-field variation of B/3F in variousastrophysical ions
Resolving power to see these lines
Detection of line B in Fe XVII
High-resolution detection of line B
B/3F depends on magnetic field and electron density