A Study of the May 13th, 2005 Two Ribbon Flare in UV and HXR

1
A Study of the May 13th, 2005 Two Ribbon Flare in
UV and HXR

• Kristin Rosenau
• Solar Physics REU 2009
• Advisers Jiong Qiu
• Maria Kazachenko

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Presentation Outline

• Introduction
• Magnetic Reconnection 
• Motivations
•  
•  Observations Data Analysis
• UV, HXR, and Reconnection Rate
• Evolution stages
•  
• Results
•  
• Conclusions

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Magnetic Reconnection
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Magnetic Reconnection 3D
Front view
Rate of magnetic reconnection is the rate flare
ribbons expand across magnetic field lines
Top view
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Measuring Reconnection Rate
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UV Evolution
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HXR Solar Flare Evolution
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UV HXR Light curves
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Determining Evolution Stages
1
2b
2a

Peak
4a
3
4b
10
Time Profiles for Significant Poles
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Scatter Plot of UV, HXR, Reconnection Rate

• Rougly linear correlation
• During rise and decay, non-thermal energy release
  per unit flux is low (less steep).
• During the peak, non-thermal energy release per
  unit flux is high (steep).

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Conclusions

• Observations
•  UV exhibits ribbon structure before and after
  the peak
• HXR kernels only show ribbon structure after the
  peak 
•  
•  

However, once spatially and temporally resolved,
we see that HXR expands along flare ribbons with
UV.
Resolution  By comparing UV, HXR, and
reconnection rate, the spatially resolved energy
release rate can be derived.
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Acknowledgments

• A special thanks to the following people for the
  advice and guidance with this project
•  
• Jiong Qiu 
• Maria Kazachenko  
• MSU Solar Physics Collaboration
• National Science Foundation (NSF)