Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002padeu..12...13m&link_type=abstract
2nd Workshop of Young Researchers in Astronomy & Astrophysics, Publications of the Astronomy Department of the Eötvös University
Astronomy and Astrophysics
Astrophysics
Scientific paper
The transition region blinkers are one of the most controversial phenomena in the lower solar atmosphere observed in the past five years. According to our model these small-scale bright intensity enhancements may play a significant role not only in the solar transition region but even in the solar wind acceleration and the solar atmospheric plasma heating. They were mainly found, e.g., in HeI (584.33A), OIII (599.52A), OIV (554.52A), OV (629.73A) and MgIX (368.06A), respectively (Harrison). Their typical parameters are: the mean lifetime is approximately 16 s, the intensity enhancement ratios are around 1.8, and the appearing frequency on the whole solar surface is at 1 - 20 1/s. Blinker events appear to be increases in density 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 regions where one magnetic polarity dominates. We have developed a simple physical model of blinkers based on the process of magnetic reconnection (Priest). In the present paper we show our results of solving the fully nonlinear, time-dependent, dissipative, radiative 2-D MHD equations using a staggered mesh. By setting the initial parameters describing blinkers we found propagating jets with similar properties found by observations.
Erdelyi Robert
Marik Daniel
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