Photoionization of cool MHD disk winds |
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Authors: | AI Gómez de Castro C Ferro-Fontán |
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Institution: | 1. Instituto de Astronomía y Geodesia (CSIC-UCM), Facultad de CC Matemáticas Universidad Complutense de Madrid, 28040, Madrid, Spain 2. Instituto de Física del Plasma (CONICET-UBA), Facultad de CC. Exactas y Naturales, Universidad de Buenos Aires, Argentina
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Abstract: | 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 ? 80,000 K) and dense (ne ? 109 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 ~ 5 × 104 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. |
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