UV spectra of T Tauri stars from Hubble Space Telescope: RW Aur

Details UV spectra of T Tauri stars from Hubble Space Telescope: RW Aur UV spectra of T Tauri stars from Hubble Space Telescope: RW Aur

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...357..951e&link_type=abstract

Astronomy and Astrophysics, v.357, p.951-956 (2000)

Astronomy and Astrophysics

Astrophysics

12

Stars: Pre-Main Sequence, Stars: Individual: Rw Aur, Ultraviolet: Stars, X-Rays: Stars

Scientific paper

Ultraviolet spectra of the classical T Tauri star RW Aur A observed with the Hubble Space Telescope were analysed. Absorption lines of neutral and singly ionized metals, blueshifted ~ 50 km s-1 relative to the star, were found. They originate in a dense (N>1010 cm-3) gas outflow, whose extension along the line of sight is less than 3R_*. The gas temperature of the wind is definitely below 10 000 K, but metals (and probably sulfur) are almost completely singly ionized by strong stellar emission in the hydrogen lines of the Lyman series. Stellar Ly_alpha quanta are responsible for a significant population of hydrogen upper levels. Their photoionization is the main source of free electrons and subsequent gas heating. Strong fluorescent lines of H_2 and Fe ii pumped by stellar Ly_alpha quanta were found in the RW Aur spectra. The emission in C iv and Si iv lines is strongly suppressed by Fe ii and Ni ii wind absorption features. Superposition of strong H_2 emission lines onto residual profiles additionally disturbs the picture, so C iv and Si iv line fluxes derived from low resolution IUE spectra are erroneous. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS\,5-26555.

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