34th Solar Physics Division Meeting, June 2003
Session 16 Flares and Microflares II
Poster, Wednesday, June 18, 2003, 3:30-5:00pm, Mezzanine

[Previous] | [Session 16] | [Next]


[16.17] Comparison of Blinkers and Explosive Events

D. Bewsher (ESA Space Science Department, NASA/GSFC), D. Innes (MPI fur Aeronomie, Germany), C.E. Parnell (Mathematical Institute, U. St Andrews, Scotland)

There has been much speculation over recent years as to whether blinkers and explosive events are the same phenomena observed with different instruments.

Blinkers were first observed by Harrison (1997) by eye using SOHO/CDS, but more recently Brkovic et al. (2001) and Bewsher et al. (2002) have developed automated methods of identifying these events. Blinkers are small scale intensity enhancements seen in the transition region, with a mean area of 3 x 107 km2 and a mean lifetime of 16 minutes. The Doppler velocities of blinkers are preferentially more red-shifted than the typical transition region plasma. The range of these enhanced velocities, however, are no larger than the typical spread of Doppler velocities in these regions.

Explosive events were first observed using HRTS (Bruckener and Bartoe, 1983) as high energy turbulent events and jets. More recently, they have been observed using SOHO/SUMER. They have a typical size of 2" - 4" and have an average lifetime of 60 seconds. Line profiles of explosive events show strong non-Gaussian enhancements of both wings of the profile, and velocities associated with them range from ± 50 - ±250 km s-1.

Examples will be presented showing (i) a co-spatial and co-incident blinker and explosive event; (ii) a blinker with no associated explosive event; and (iii) an explosive event with no associated blinker. We investigate the lightcurves and line profiles of the regions to explain the relationship, if any, between blinkers and explosive events.


[Previous] | [Session 16] | [Next]

Bulletin of the American Astronomical Society, 35 #3
© 2003. The American Astronomical Soceity.