Solar flares and Coronal Mass Ejections (CMEs) are two types of solar phenomena that occur in intense magnetic regions of our Sun. Both involve the fast release of magnetic energy and produce large-scale perturbations throughout the solar atmosphere. The energy release mechanism generally believed to be responsible for both of these phenomena is magnetic reconnection.

Certain mathematical models have been proposed for flares and CMEs that require the presence of a null point in the solar atmosphere. Unfortunately, given current observation techniques, it is almost impossible to observe these coronal nulls directly. An alternative approach is to combine magnetic observations and 3D modelling methods to extrapolate the coronal magnetic field from the field of the photosphere of an active region. We can then determine its magnetic topology, in particular the locations of the null points.

In this project we are concerned with the topology of the observed magnetic field of active-region AR0486 during a period of intense solar activity. By considering an extrapolation of data obtained from SOHO/MDI and Hinode/SOT photospheric magnetograms using the magnetic field extrapolation tools developed by S. Regnier et al. (2002, 2006), and by employing the 'null point finding code' created by Haynes et al. (2007) in conjunction with various analysis programs developed during this project by the author (2008), we undertake an analysis of the physical character and behaviour of the magnetic null points discovered in that region. Our motivating question is whether coronal null points are a necessary requirement for flares or CMEs. It is hoped that the details of this study may have something to contribute towards an answer to this question.