@Article{LoeschOphAlvEvaMan:2011:SiTwDi,
               author = "Loesch, C. and Opher, Merav and Alves, Maria Virginia and Evans, 
                         R. M. and Manchester, W. B.",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and George 
                         Mason Univ, Dept Phys \& Astron, Fairfax, VA 22030 USA and 
                         {Instituto Nacional de Pesquisas Espaciais (INPE)} and George 
                         Mason Univ, Dept Phys \& Astron, Fairfax, VA 22030 USA and Univ 
                         Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48108 USA",
                title = "Signatures of two distinct driving mechanisms in the evolution of 
                         coronal mass ejections in the lower corona",
              journal = "Journal of Geophysical Research",
                 year = "2011",
               volume = "116",
                pages = "A04106",
                month = "Apr.",
             keywords = "MAGNETIC-FLUX TUBES, SOLAR-WIND, MAGNETOHYDRODYNAMIC MODEL, 
                         INTERPLANETARY SHOCKS, SHEATH STRUCTURES, ROPE, ACCELERATION, 
                         SIMULATION, CME, PROPAGATION.",
             abstract = "We present a comparison between two simulations of coronal mass 
                         ejections (CMEs), in the lower corona, driven by different flux 
                         rope mechanisms presented in the literature. Both mechanisms 
                         represent different magnetic field configurations regarding the 
                         amount of twist of the magnetic field lines and different initial 
                         energies. They are used as a {"}proof of concept{"} to explore how 
                         different initialization mechanisms can be distinguished from each 
                         other in the lower corona. The simulations are performed using the 
                         Space Weather Modeling Framework (SWMF) during solar minimum 
                         conditions with a steady state solar wind obtained through an 
                         empirical approach to mimic the physical processes driving the 
                         solar wind. Although the two CMEs possess different initial 
                         energies (differing by an order of magnitude) and magnetic 
                         configurations, the main observables such as acceleration, shock 
                         speed, Mach number, and theta(Bn) (the angle between the shock 
                         normal and the upstream magnetic field) present very similar 
                         behavior between 2 and 6 R(circle dot). We believe that through 
                         the analysis of other quantities, such as sheath width and 
                         postshock compression (pileup and shock indentation compressions), 
                         the effect of different magnetic configurations and 
                         initializations can be distinguished. We discuss that coronal 
                         models that employ a reduced value of polytropic index (gamma) may 
                         significantly change the energetics of the CME and that the 
                         background solar wind plays an important role in the CMEs' shock 
                         and sheath evolution.",
                  doi = "10.1029/2010JA015582",
                  url = "http://dx.doi.org/10.1029/2010JA015582",
                 issn = "0148-0227 and 2156-2202",
                label = "lattes: 6460301165792800 3 LoeschOphAlvEvaMan:2011:SiTwDi",
             language = "en",
           targetfile = "2010JA015582.pdf",
        urlaccessdate = "20 abr. 2024"
}