2026-06-08T22:08:06Zhttps://docta.ucm.es/rest/oai/requestoai:docta.ucm.es:20.500.14352/500732024-07-11T13:52:03Zcom_20.500.14352_14col_20.500.14352_15
Evidence for an ionized rotating structure around RW Aur
Gómez De Castro, Ana Inés
Verdugo, Eva
52
T tauri stars
Spectrograph observations
Transition region
Emission-line
Young stars
Asymmetries
Accretion
Aurigae
Jet
Chromosphere
Stars
Pre-main-sequence
T Tauri
Individual
RW aur
Astronomía (Matemáticas)
21 Astronomía y Astrofísica
International Workshop on Magnetic Fields and Star Formation, APR 21-25, 2003, Madrid, SPAIN
Profiles of the UV semiforbidden lines of C III](1908) and Si III](1892) of RW Aur have been obtained with the HST/STIS. The C III](1908) profile shows two high velocity components at v = +/- 170 km s(-1) and a central one. The Si III](1892) 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) similar or equal to 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.
Unidad Deptal. de Astronomía y Geodesia
Fac. de Ciencias Matemáticas
TRUE
pub
2023-06-20T09:37:54Z
2023-06-20T09:37:54Z
2004
journal article
https://hdl.handle.net/20.500.14352/50073
0004-640X
10.1023/B:ASTR.0000045076.14133.89
eng
Gómez De Castro, A. I. & Verdugo, E. «Evidence for an Ionized Rotating Structure Around RW Aur». Astrophysics and Space Science, vol. 292, n.o 1-4, 2004, pp. 691-96. DOI.org (Crossref), https://doi.org/10.1023/B:ASTR.0000045076.14133.89.
restricted access
application/pdf
Springer