@Article{BorgazziLaraEcheAlve:2009:DyCoMa,
               author = "Borgazzi, Andrea and Lara, A. and Echer, Ezequiel and Alves, Maria 
                         Virg{\'{\i}}nia",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {} and 
                         {Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)}",
                title = "Dynamics of coronal mass ejections in the interplanetary medium",
              journal = "Astronomy \& Astrophysics",
                 year = "2009",
               volume = "498",
               number = "3",
                pages = "885--889",
                month = "May",
             keywords = "hydrodynamics, Sun: coronal mass ejections (CMEs), interplanetary 
                         medium.",
             abstract = "Context. Coronal mass ejections (CMEs) are large plasma structures 
                         expelled from the low corona to the interplanetary space with a 
                         wide range of speeds. In the interplanetary medium CMEs suffer 
                         changes in their speeds because of interaction with the ambient 
                         solar wind. Aims. To understand the interplanetary CME (ICME) 
                         dynamics, we analyze the interaction between these structures and 
                         the ambient solar wind (SW), approaching the problem from the 
                         hydrodynamic point of view. Methods. We assume that the dynamics 
                         of the system is dominated by two kinds of drag-force dependence 
                         on speed (U), as similar to U and similar to U-2. Furthermore, we 
                         propose a model that takes variations of the ICME radius (R) and 
                         SW density (rho(sw)) into account as a function of the distance 
                         (x) as R(x) = x(0.78) and rho(sw)(x) = 1/x(2), respectively. Then, 
                         we solve the equation of motion and present exact solutions. 
                         Results. Considering CME speeds measured at a few solar radii and 
                         at one AU, we were able to constrain the values of the constants 
                         (viscosity and drag coefficient) for the linear (U) and quadratic 
                         (U-2) speed dependences, which seems to reproduce the ICME-SW 
                         system well. We found different solutions in which the concavity 
                         of the curves of the ICME speed profile changes, depending on the 
                         dominant factor, either the ICME radius or the SW density. 
                         Conclusions. This work shows that the macroscopic ICME propagation 
                         may be described by the hydrodynamic theory and that it is 
                         possible to find analytical solutions for the ICME-SW 
                         interaction.",
                  doi = "10.1051/0004-6361/200811171",
                  url = "http://dx.doi.org/10.1051/0004-6361/200811171",
                 issn = "0004-6361 and 1432-0746",
             language = "en",
           targetfile = "A9RE.tmp.pdf",
        urlaccessdate = "08 maio 2024"
}