@misc{SuKliemvanBallegooijenetal.2012,
  author    = {Su, Yingna and Kliem, Bernhard and van Ballegooijen, Adriaan and Deluca, Edward},
  title     = {Numerical simulations of the CME on 2010 April 8},
  series = {Solar and Astrophysical Dynamos and Magnetic Activity},
  journal   = {Solar and Astrophysical Dynamos and Magnetic Activity},
  number    = {674},
  issn      = {1866-8372},
  doi       = {10.25932/publishup-41488},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-414887},
  pages     = {575 -- 576},
  year      = {2012},
  abstract  = {We present 3D zero-beta ideal MHD simulations of the solar flare/CME event that occurred in Active Region 11060 on 2010 April 8. The initial magnetic configurations of the two simulations are stable nonlinear force-free field and unstable magnetic field models constructed by Su et al. (2011) using the flux rope insertion method. The MHD simulations confirm that the stable model relaxes to a stable equilibrium, while the unstable model erupts as a CME. Comparisons between observations and MHD simulations of the CME are also presented.},
  language  = {en}
}
@misc{GreenKliem2013,
  author    = {Green, Lucie M. and Kliem, Bernhard},
  title     = {Observations of flux rope formation prior to coronal mass ejections},
  series = {Postprints der Universit{\"a}t Potsdam : Mathematisch-Naturwissenschaftliche Reihe},
  journal   = {Postprints der Universit{\"a}t Potsdam : Mathematisch-Naturwissenschaftliche Reihe},
  number    = {607},
  issn      = {1866-8372},
  doi       = {10.25932/publishup-41610},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-416103},
  pages     = {6},
  year      = {2013},
  abstract  = {Understanding the magnetic configuration of the source regions of coronal mass ejections (CMEs) is vital in order to determine the trigger and driver of these events. Observations of four CME productive active regions are presented here, which indicate that the pre-eruption magnetic configuration is that of a magnetic flux rope. The flux ropes are formed in the solar atmosphere by the process known as flux cancellation and are stable for several hours before the eruption. The observations also indicate that the magnetic structure that erupts is not the entire flux rope as initially formed, raising the question of whether the flux rope is able to undergo a partial eruption or whether it undergoes a transition in specific flux rope configuration shortly before the CME.},
  language  = {en}
}