@InProceedings{BarbosaAlveSimõ:2016:PISiTh,
               author = "Barbosa, Marcos Vinicius Grala and Alves, Maria Virginia and 
                         Sim{\~o}es J{\'u}nior, Fernando",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Universidade Federal 
                         de Pelotas (UFPel)}",
                title = "PIC simulations of a three component plasma described by Kappa 
                         distribution functions as observed in Saturn’s magnetosphere",
            booktitle = "Abstracts...",
                 year = "2016",
         organization = "European Geophysical Society General Assembly",
             abstract = "In plasmas out of thermodynamic equilibrium the particle velocity 
                         distribution can be described by the so called Kappa distribution. 
                         These velocity distribution functions are a generalization of the 
                         Maxwellian distribution. Since 1960, Kappa velocity distributions 
                         were observed in several regions of interplanetary space and 
                         astrophysical plasmas. Using KEMPO1 particle simulation code, 
                         modified to introduce Kappa distribution functions as initial 
                         conditions for particle velocities, the normal modes of 
                         propagation were analyzed in a plasma containing two species of 
                         electrons with different temperatures and densities and ions as a 
                         third specie.This type of plasma is usually found in 
                         magnetospheres such as in Saturn. Numerical solutions for the 
                         dispersion relation for such a plasma predict the presence of an 
                         electron-acoustic mode, besides the Langmuir and ion-acoustic 
                         modes. In the presence of an ambient magnetic field, the 
                         perpendicular propagation (Bernstein mode) also changes, as 
                         compared to a Maxwellian plasma, due to the Kappa distribution 
                         function. Here results for simulations with and without external 
                         magnetic field are presented. The parameters for the initial 
                         conditions in the simulations were obtained from the Cassini 
                         spacecraft data. Simulation results are compared with numerical 
                         solutions of the dispersion relation obtained in the literature 
                         and they are in good agreement.",
  conference-location = "Vienna, Austria",
      conference-year = "17-22 Apr.",
             language = "en",
                  ibi = "8JMKD3MGP3W34P/3LR5K48",
                  url = "http://urlib.net/ibi/8JMKD3MGP3W34P/3LR5K48",
           targetfile = "barbosa_pic.pdf",
        urlaccessdate = "27 abr. 2024"
}