1 / 13

Line Profile Characteristics of Solar Explosive Event Bursts

Line Profile Characteristics of Solar Explosive Event Bursts. Z. Ning et al 2004 A&A 419,1141. Speaker: Jinping Dun. 1. Introduction. Explosive Event is a small-scale, short-lifetime phenomenon in the transition region of quiet Sun. Main Characteristics Broaden Line Profile

elvis-reid
Download Presentation

Line Profile Characteristics of Solar Explosive Event Bursts

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Line Profile Characteristics of Solar Explosive Event Bursts Z. Ning et al 2004 A&A 419,1141 Speaker: Jinping Dun

  2. 1. Introduction • Explosive Eventis a small-scale, short-lifetime phenomenon in the transition region of quiet Sun. • Main Characteristics Broaden Line Profile T ~ 105K ( i.e. SiIV 1393 Å) V~100km/s Size ~ 2” Lifetime ~ 1min • Physical Model Plasma Jets Produced by Magnetic Reconnection

  3. 2. Observations and Data Reduction (i) • MDI Magnetogram The area rastered by SUMER and locations of explosive events

  4. 2. Observations and Data Reduction (ii) • SiIV 1393 Å Spectrum Slit ~ 1” x120” Step ~ 6 Interval~ 1.13” Exposure Time ~5s

  5. 3.Examples and Results (i) • Time Variation of Integrated Intensity

  6. 3.Examples and Results (ii) • Repetition of Explosive Events

  7. 3.Examples and Results (iii) • 2D Time Evolution of 5 Groups of Events The black dashed line boxes surround events with obvious red-blue wing spatial offset. (Evidence of reconnection jets, Innes et al.,1997, Nature,386,811)

  8. 3.Examples and Results (iv) • The Magnetic Field Emergence (white) and Cancellation (black)

  9. 4.Discussion • 2D Structure Evolution of Explosive Events • Repetition of Explosive Events Magnetic reconnection could be triggered by 3~5 min oscillation waves in the chromospheric and transition region.

  10. Thank You！

  11. Profile of Explosive Event (i) Velocity Along Line-of-sight V=0 Explosive Event V<0(blue-Shift) V>0(red-shift) Wavelength

  12. Profile of Explosive Event (ii) SiIV 1393.78 Ni 1393.33

  13. Profile of Explosive Event (iii) stationary component red-shift components blue-shift component three components: stationary and two high-speed (along line-of-sight) sources. (Chae et al.1998,ApJ,497,L109)

More Related