Volume 395, Number 3, December I 2002
|Page(s)||977 - 981|
|Section||Planets and planetary systems|
|Published online||18 November 2002|
Microflaring of a solar bright point*
Observatory, Box 14, 00014 University of Helsinki, Finland e-mail: firstname.lastname@example.org;
2 Tuorla Observatory, University of Turku, Finland e-mail: email@example.com
3 Max-Planck-Institut für Aeronomie, 37191 Katlenburg-Lindau, Germany e-mail: firstname.lastname@example.org
Corresponding author: O. Vilh, email@example.com
Accepted: 11 July 2002
A arcsec region near the solar disc center containing a bright point (BP) was observed with the SUMER- spectrograph of the SOHO observatory. The data consist of two hours observation of four far-UV emission lines formed between – K, with 2 arcsec spatial, 2.8 min temporal and 4 km s-1 spectral resolution. A striking feature was the strong microflaring of the major persistent BP (with size arcsec) and the appearance of several short lived transients. The microflaring of each individual arcsec pixel inside the main BP was coherent, indicating strong interaction of the possible sub arc sec building blocks (magnetic flux tubes). Using the emission measure at 105 K as an indicator of the loop foot point area and magnetic filling factor, we suggest 10 per cent filling factor for the BP observed. This is similar to that on the average surface of a medium-active solar type star.
Key words: Sun: UV radiation / Sun: chromosphere / Sun: transition region / Sun: corona / stars: activity
© ESO, 2002
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