Ferro-Fontán, C. y Gómez de Castro, Ana Inés (2003) Photoionization of cool MHD diskwinds - On the source of the far UV emission lines from T Tauri stars. Astrophysics and space science, 287 . pp. 31-34. ISSN 0004-640X
Recent ultraviolet observations point out that there is hot, dense plasma associated with the optical jet in some T Tauri stars. In this contribution, cool MHD disk wind physics is reviewed by means of a self-similar analytical model to analyze whether hot (Te similar or equal to 80, 000 K) and dense (n(e) similar or equal to 10(9) cm(-3)) plasma can be produced in disk winds. It is shown that these high densities can only be achieved at the base of the wind where the stellar X-rays radiation field is strong. The propagation of the X-rays radiation through the disk wind is analyzed: a cocoon of photoionized gas is generated around the star. However, it is difficult to foresee how temperatures as high as similar to5 x 10(4) can be reached unless a significant fraction of the X-rays radiation is produced by magnetic reconnection at the boundary between the stellar magnetosphere and the accretion disk.
|Tipo de documento:||Artículo|
|Palabras clave:||Accretion-ejection structures;|
|Materias:||Ciencias > Matemáticas > Astronomía|
|Depositado:||17 Sep 2012 10:26|
|Última Modificación:||17 Sep 2012 10:26|
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