Physics
Scientific paper
Jun 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508..315m&link_type=abstract
In: Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 11-15 March 2002, Davos, Switze
Physics
Explosive Events, Blinkers, Magnetic Reconnection
Scientific paper
The transition region blinkers, according to the present model, may play a significant role not only in the solar transition region and the solar atmospheric plasma heating but may even contribute to the solar wind mass flux. They were mainly found, e.g., in He I, O III, O IV, O V and Mg IX, respectively (Harrison, 1997). Their typical lifetime is approximately 16s, the intensity enhancement ratios are around 1.8, and they appear at 1 - 20 s-1 on the Sun. Blinker events seem to be increases in density and/or filling factor rather then to be increases in temperature. Most of the blinkers have repetitive nature and high percentage of these events occur above unipolar magnetic field. A simple physical model of blinkers based on the process of magnetic reconnection is developed. In the present paper results of solving the fully nonlinear, time-dependent, dissipative, radiative 2-D MHD equations are shown. By setting the initial parameters describing blinkers and taking into account the limit of the spatial resolution of SOHO CDS propagating reconnection jets are found to have properties described by CDS observations. Results may suggest SOHO CDS observes explosive events as blinkers in some cases.
Erdelyi Robert
Marik Daniel
No associations
LandOfFree
What blinkers really are? does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with What blinkers really are?, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and What blinkers really are? will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1210846