Eruption of magnetic flux ropes during flux emergence

V. Archontis, T. Torok

Research output: Contribution to journalArticlepeer-review

120 Citations (Scopus)

Abstract

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.

Original languageEnglish
Number of pages4
JournalExperimental Astronomy
Volume492
DOIs
Publication statusPublished - Dec 2008

Keywords

  • magnetohydrodynamics (MHD)
  • methods: numerical
  • Sun: activity
  • Sun: corona
  • Sun: magnetic fields
  • CORONAL MASS EJECTIONS
  • HELICITY BUDGET
  • EMERGING FLUX
  • FIELD
  • KINK
  • ACCELERATION
  • FILAMENT
  • REGIONS

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