Volume 468, Number 2, June III 2007
The XMM-Newton extended survey of the Taurus molecular cloud
|Page(s)||541 - 556|
|Published online||19 December 2006|
The first high-resolution X-ray spectrum of a Herbig star: AB Aurigae
Paul Scherrer Institut, Würenlingen and Villigen, 5232 Villigen PSI, Switzerland e-mail: [atellesc;guedel;briggs]@astro.phys.ethz.ch
2 Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309-0389, USA e-mail: firstname.lastname@example.org
3 Columbia Astrophysics Laboratory, Mail Code 5247, 550 West 120th Street, New York, NY 10027, USA e-mail: email@example.com
4 INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: firstname.lastname@example.org
Accepted: 11 October 2006
Context.The X-ray emission from Herbig Ae/Be stars remains to be explained. In later-type T Tauri stars, X-rays are thought to be produced by magnetically trapped coronal plasma, although accretion-shock induced X-rays have also been suggested. In earlier-type (OB) stars, shocks in unstable winds are thought to produce X-rays.
Aims.We present the first high-resolution X-ray spectrum of a prototypical Herbig star AB Aurigae), measure and interpret various spectral features, and compare our results with model predictions.
Methods.We use X-ray spectroscopy data from the XMM-Newton Reflection Grating Spectrometers and the EPIC instruments. The spectra are interpreted using thermal, optically thin emission models with variable element abundances and a photoelectric absorption component. We interpret line flux ratios in the He-like triplet of O vii as a function of electron density and the UV radiation field. We use the nearby co-eval classical T Tauri star SU Aur as a comparison.
Results.AB Aurigae reveals a soft X-ray spectrum, most plasma being concentrated at 1–6 MK. The He-like triplet reveals no signs of increased densities as reported for some accreting T Tau stars in the literature. There are also no clear indications of strong abundance anomalies in the emitting plasma. The light curve displays modulated variability, with a period of ≈42 h.
Conclusions.It is unlikely that a nearby, undetected lower-mass companion is the source of the X-rays. Accretion shocks close to the star would be expected to be irradiated by the photosphere, leading to alteration in the He-like triplet fluxes of O vii, which we do not measure. Also, no indications for high densities are found, although the mass accretion rate is presently unknown. Emission from wind shocks is unlikely, given the weak radiation pressure. A possible explanation would be a solar-like magnetic corona. Magnetically confined winds are a very promising alternative. The X-ray period is indeed close to periods previously measured in optical lines from the wind.
Key words: stars: coronae / stars: formation / stars: pre-main sequence / stars: magnetic fields / X-rays: stars / stars: individual: AB Aurigae
© ESO, 2007
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