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Solar Flares' Abnormal Wide Line Annihilation: Understanding the 3gamma/2gamma Ratio and Time Profile

Explore the abnormal wide annihilation line of solar flares focusing on the 3gamma/2gamma ratio, time profile, and challenges with existing models. Learn about high-energy resolution studies and the formation of wide lines at thermal temperatures. Discover the complexities of positronium formation and annihilation processes, with insights into precipitation regions and the origin of positrons. Delve into the implications of the 3gamma/2gamma ratio and time profiles in understanding solar flare dynamics and nuclear de-excitation lines.

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Solar Flares' Abnormal Wide Line Annihilation: Understanding the 3gamma/2gamma Ratio and Time Profile

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  1. The abnormal wide annihilation line of solar flares ShiChao TANG

  2. Content • Observation • Wide Line • 3gamma/2gamma ratio • Time profile • Problem with the models

  3. High Energy Resolution http://hesperia.gsfc.nasa.gov/hessi/concept.htm

  4. High Energy Resolution Share et al 2003

  5. Wide Line Thermal 6000 K

  6. Wide Line • Positronium formed via charge exchange in flight, ~6000K • Thermally broadened in a hot region with temperature of ~400000 K

  7. Annihilation

  8. 3 Gamma Continum para-positronium ortho-positronium T+, D+, ->3 gamma/2 gamma- Share 2004

  9. 3 gamma/2 gamma Share 2004

  10. 3 gamma/2 gamma 6000 K imply a ratio of ~ 3.7

  11. Time Profile Schrijver 2006

  12. Time Profile

  13. Different precipitation regions Schrijver 2006

  14. Where are they from? • In flight? • ? • Quiet Sun? • Not in equilibrium • Flare loop? • Different precipitation regions, the positrons from \beta+ decay can not go into the flare loop. • Bulk motion? • The other nuclear de-excitation lines were not broaden

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