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The contemporary multi-wavelength observations have revealed variousimportant features during solar flares which, on one hand, support thetwo-dimensional (2D) "standard flare model" while, on other hand, also urge forthe exploration of three-dimensional (3D) magnetic field topologies involved inflares. Traditionally, the formation of parallel ribbons on both side of thepolarity inversion line (PIL) and associated overlying loop arcades have beenrecognized as the most prominent features of eruptive flares which has formedthe basis for the development of the standard model providing a 2D descriptionof the flare-associated phenomena. The actual flare, however, occurs in a morecomplicated 3D magnetic structure. Thus, despite the general applicability, thestandard model has limited or no scope in explaining some of the features whichexclusively requires a 3D description. In this context, the observations of"circular ribbon flares" stand out where one of the ribbons presents an almostfully closed quasi-circular or quasi-ellipsoidal shape, evidencing theinvolvement of a typical fan-spine magnetic configuration. In this article, wediscuss observational features vis \`a vis theoretical understanding of solarflares in view of 2D and 3D models of magnetic reconnection. We highlight a fewcomplex cases of circular ribbon flares exhibiting parallel ribbons, a coronaljet, and/or an erupting magnetic flux rope. Exploring various 3D topologiesalso enables us to probe similarities between the circumstances that govern theonset of jets, confined flares and CME-producing eruptive flares.

Onset and evolution of solar flares: Application of 2D and 3D models of magnetic reconnection