New insights in the FUV into the activity of the Herbig Ae star HD 163296

Free access article

Issue		A&A Volume 429, Number 1, January I 2005


Page(s)		247 - 255
Section		Stellar structure and evolution
DOI		http://dx.doi.org/10.1051/0004-6361:20041446

A&A 429, 247-255 (2005)
DOI: 10.1051/0004-6361:20041446

New insights in the FUV into the activity of the Herbig Ae star HD 163296

M. Deleuil¹, J.-C. Bouret¹, C. Catala², A. Lecavelier des Etangs³, A. Vidal-Madjar³, A. Roberge⁴, P. D. Feldman⁵, C. Martin¹ and R. Ferlet³

¹ Laboratoire d'Astrophysique de Marseille, CNRS - Université de Provence, BP 8, 13376 Marseille Cedex 12, France
e-mail: magali.deleuil@oamp.fr
² Observatoire de Paris-Meudon, CNRS, Paris, France
³ Institut d'Astrophysique de Paris, 98bis Bd Arago, 75014 Paris, France
⁴ Dept. of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Rd., Washington, DC 20015-1305, USA
⁵ Dept. of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles St., Baltimore, Maryland 21218, USA

(Received 10 June 2004 / Accepted 28 July 2004 )

Abstract
We present an analysis of the FUSE spectra of HD 163296 , a young isolated Herbig Ae star. The spectra in the far UV spectral range are dominated by strong emission lines of $\ion{C}{iii}$ and $\ion{O}{vi}$ , which exhibit broad and complex asymmetric profiles with wings extending over more than 1000 km s ^-1. The $\ion{H}{i}$ Ly $\alpha$ and the $\ion{C}{iii}$ emission profiles show evidence for an outflow with a terminal velocity of 270 km s ^-1. We also identified several narrower emission lines due to fluorescent decays in $\ion{Fe}{ii}$ . Using an HST/STIS archive spectrum, we checked that the $\ion{H}{i}$ Ly $\alpha$ line, which has a clear type III P Cygni emission profile, is broad enough to provide the photons required to photo-excite the $\ion{Fe}{ii}$ upper levels. As previously explored for the well-known Herbig Ae star AB Aur , most of the spectral features including the fluorescent lines are consistent with the presence of a chromosphere above the photosphere. However, the over-ionized species cannot be produced in this region alone and we discuss two alternative mechanisms to explain such spectral signatures: magnetospheric accretion and a magnetically confined wind. Both interpretations involve a large-scale magnetic field whose detection is now a challenge for the new generation of spectropolarimeters such as ESPaDOnS.

Key words: stars: activity -- stars: individual: HD 163296 -- line: profiles -- line: identification -- stars: magnetic fields

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