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Evidence for an ionized rotating structure around RW Aur



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Gómez de Castro, Ana Inés y Verdugo, Eva (2004) Evidence for an ionized rotating structure around RW Aur. Astrophysics and space science, 292 . pp. 691-696. ISSN 0004-640X

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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.

Tipo de documento:Artículo
Información Adicional:

International Workshop on Magnetic Fields and Star Formation, APR 21-25, 2003, Madrid, SPAIN

Palabras clave:T tauri stars; spectrograph observations; transition region; emission-line; young stars; asymmetries; accretion; aurigae; jet; chromosphere; stars : pre-main-sequence; stars : T tauri; stars : individual : RW aur
Materias:Ciencias > Matemáticas > Astronomía
Código ID:16114
Depositado:31 Jul 2012 08:29
Última Modificación:26 Jun 2018 07:40

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