Magnetic-field variations in the active region NOAA 10486 and their relationship to X-ray flares and coronal mass ejections

Details Magnetic-field variations in the active region NOAA 10486 and their relationship to X-ray flares and coronal mass ejections Magnetic-field variations in the active region NOAA 10486 and their relationship to X-ray flares and coronal mass ejections

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008arep...52..852c&link_type=abstract

Astronomy Reports, Volume 52, Issue 10, pp.852-865

Astronomy and Astrophysics

Astronomy

2

96.60.Qe, 96.60.Ph, 96.60.Hv, 96.60.Tf

Scientific paper

SOHO/MDI magnetograms are used to analyze the time variations in the magnetic parameters of the active region (AR) NOAA 10486, which was part of a large activity complex that passed over the solar disk from October 26 to 31, 2003, during solar cycle 23. The results are compared with X-ray flares in the AR and the parameters of coronal mass ejections associated with the AR. The time variations in the distributions of themagnetic-field strengths associated with the total magnetic flux (Fa), the flux imbalance between the northern and southern polarities (Im), the complexity of the field, as a measure of the mutual overlapping of the opposite polarities (Co), and the tilt angle of the magnetic axis (An) are considered. The time variations in the free energy accumulated in current sheets of ARs were traced using a parameter introduced for this purpose (Sh). The following results were obtained. First, the parameters Fa, Im, Co, An, and Sh quantitatively describe the current state of the AR and can be used to trace and analyze the dynamical evolution of its magnetic field. Second, variations in the magnetic-field-strength distributions and the mean values of Fa, Im, Co, An, and Sh are associated with flares and coronal mass ejections, and the variations have considerable amplitudes. Third, the parameter Sh characterizing the degree to which the magnetic field is non-potential in regions adjacent to the main neutral line increases before eruptive events, and is thus particular interest for monitoring the states of ARs in real time. Fourth, the magnetic field of the AR manifests a sort of quasi-elasticity, so that the field structure is restored after active events, on average, within 1 3 h.

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