Franqueira, M.Tagger, M.Gómez de Castro, Ana Inés2023-06-202023-06-202004Franqueira, M., Tagger, M. and G´omez de Castro, A. I.: 2000, A&A 357, 1143. Haerendel, G.: 1992, Nat. 360, 241. Haffner, L.M., Reynolds, R.J. and Tufte, S.L.: 1998, ApJ 501, L83. Kulsrud, R. and Pearce, W.: 1969, ApJ 156, 445. McIvor, I.: 1977, MNRAS 178, 85. Mestel, L. and Spitzer, L.: 1956, MNRAS 116, 503. Minter, A.H. and Spangler, S.R.: 1996, ApJ 458, 194. Minter, A.H. and Spangler, S.R.: 1997, ApJ 485, 182. Piddington, J.H.: 1956, MNRAS 116, 314. Reynolds, R.J., Haffner, L.M. Tufte, S. L.: 2000, in: J. Arthur, N. Brickhouse, and J. Franco (eds.), Astrophysical plasmas: Codes, Models and Observations, Rev. Mex. Astron. Astrof. (Serie de conferencias) Vol. 9, p. 249. Tagger, M., Falgarone, E. and Shukurov, A.: 1995, A&A 229, 940.0004-640X10.1023/B:ASTR.0000045012.41087.07https://hdl.handle.net/20.500.14352/50069International Workshop on Magnetic Fields and Star Formation, APR 21-25, 2003, Madrid, SPAINWe present the 2-D, two fluid ( ions + neutrals) numerical simulations that we are carrying out in order to study the ambipolar filamentation process, in which a magnetized, partially ionized plasma is stirred by turbulence in the ambipolar frequency range. The higher turbulent velocity of the neutrals in the most ionized regions gives rise to a non-linear force driving them out of these regions, and causes the ions and the magnetic flux to condense in the most ionized regions, resulting in a filamentary structure where initial ionization inhomogeneities are amplified. This mechanism might help to explain some features observed in magnetized and partially ionized astrophysical plasmas as the interstellar medium.engjournal articlehttp://www.springerlink.com/content/w2x150550n3157m0/fulltext.pdfhttp://www.springerlink.com/open access52Turbulent magnetic-fieldswavesmagnetohydrodynamicsturbulenceISM : magnetic fieldsnumerical methodsAstronomía (Matemáticas)21 Astronomía y Astrofísica