Eruption of magnetic flux ropes during flux emergence

By V. Archontis, T. Torok. 2008

137 citations recorded by the source corpus.

Aims. We investigate the formation of flux ropes in a flux emergence region and their rise into the outer atmosphere of the Sun. Methods. We perform 3D numerical experiments by solving the time-dependent and resistive MHD equations. Results. A sub-photospheric twisted flux tube rises from the solar interior and expands into the corona. A flux rope is formed within the expanding field, due to shearing and reconnection of field lines at low atmospheric heights. If the tube emerges into a non-magnetized atmosphere, the flux rope rises, but remains confined inside the expanding magnetized volume. In contrast, if the expanding tube is allowed to reconnect with a pre-existing coronal field, the flux rope experiences a full eruption with a rise profile that is in qualitative agreement with erupting filaments and Coronal Mass Ejections.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2cab845224ab2bfbdb74e0653328d23bad2648d1

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In Astronomy and Astrophysics

Citations in the corpus

Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, background): “Examples include: shearing motions (Antiochos et al., 1994), emergence of the upper part of a flux rope (Manchester et al., 2004; Archontis and Török, 2008; DeVore and Antiochos, 2000; Fan, 2009) or shearing motions followed by convergence and cancellation of photospheric flux (van Ballegooijen…”