Evidence for an Ionized Rotating Structure Around RW Aur
- 31 Downloads
Profiles of the UV semiforbidden lines of C III and Si III of RW Aur have been obtained with the HST/STIS. The C III profile shows two high velocity components at v = ± 170 km s−1 and a central one. The Si III profile is very broad (FWHM = 293 km s−1) and the high velocity components are unresolved. It is shown that the high velocity components are most probably produced in a rotating belt alike the detected in other sources of bipolar outflows. A radius between 2.7 R * and the corotation radius (6.1 R *) is derived and a log T e (K) ≃4.7 and log n e(cm −3) = 11.6 are estimated. The belt is clumpy and the most likely source of heating is local X-rays radiation, probably associated with the release of magnetic energy.
Unable to display preview. Download preview PDF.
- Gómez de Castro, A.I. and Franqueira, M.: 1997, ULDA Access Guide to T Tauri stars observed with IUE, ESA-SP 1205, ESA Publisher, Noordwijk, The Netherlands.Google Scholar
- Gómez de Castro, A.I. and Verdugo, E.: 2002, Highlights of Spanish Astrophysics, III Dordrecht: Kluwer Academic Publishers, Gallego, J., Zemoreno, J. and Cardiel, N. (eds.), p. 361.Google Scholar
- López-Martín, L., Cabrit, S. and Dougados, C.: 2003, A& A 405, L1.Google Scholar