F. Tomasz1,
S. Regnier2,
P. Schwartz3,
J. Rybák1,
A. Kucera1,
P. Heinzel3,
W. Curdt4,
H. Wöhl5
1Astronomical Institute of the Slovak Academy of Sciences,
SK-05960 Tatranská Lomnica, Slovakia
2Institute of Mathematics, University of St. Andrews, St. Andrews, United Kingdom
3Astronomical Institute, Academy of Sciences of the Czech Republic, Ond^rejov, Czech Republic
4Max-Planck-Institut für Aeronomie, D-37189 Katlenburg-Lindau, Germany
5Kiepenheuer-Institut für Sonnenphysik, D-79104 Freiburg, Germany
We report on theoretical modeling of an eruptive event observed by SoHO/SUMER in H I Lyman beta 1025.72 A, C II 1037.00 A and O VI 1037.64 A emission of the quiet so-lar atmosphere. We are using two different theoretical approaches. The first one is based on the application of thecloud model to a loop hanging in the solar atmosphere and being irradiated by incident photospheric and chromospheric emissions. This model gives spectral profiles of the hydrogen Lyman beta line that are in good quantitative agreement with the observations. The second approach is based on potential-field extrapolation of the photospheric magnetic field as from SoHO/MDI line-of-sight magnetograms into the upper layers of the solar atmosphere. Here, the aim was to find evidence for a possible magnetic reconnection process responsible for the energy release during the observed event. We found that the event is located closely to a separator field line intersecting twoseparatrix surfaces which evidence the possible magnetic reconnection process. The typical height of the loop systems derived from magnetic field extrapolation is in good agreement with the top height of the eruptive event struc-ture computed from the cloud model. Finally, two possible scenarios of the eruptive event are proposed.
Back to the list of the non-refereed contributions
File of the contribution (pdf)