SIMBAD references

2011MNRAS.417..472D - Mon. Not. R. Astron. Soc., 417, 472-487 (2011/October-2)

The large-scale magnetic field and poleward mass accretion of the classical T Tauri star TW Hya.

DONATI J.-F., GREGORY S.G., ALENCAR S.H.P., BOUVIER J., HUSSAIN G., SKELLY M., DOUGADOS C., JARDINE M.M., MENARD F., ROMANOVA M.M., UNRUH Y.C. (The MaPP collaboration)

Abstract (from CDS):

We report here results of spectropolarimetric observations of the ≃ 8 Myr classical T Tauri star (cTTS) TW Hya carried out with ESPaDOnS at the Canada–France–Hawaii Telescope in the framework of the `Magnetic Protostars and Planets' programme, and obtained at two different epochs (2008 March and 2010 March). Obvious Zeeman signatures are detected at all times, both in photospheric lines and in accretion-powered emission lines. Significant intrinsic variability and moderate rotational modulation are observed in both photospheric and accretion proxies.

Using tomographic imaging, we reconstruct maps of the large-scale field of the photospheric brightness and the accretion-powered emission at the surface of TW Hya at both epochs. We find that the magnetic topology is mostly poloidal and axisymmetric with respect to the rotation axis of the star and that the octupolar component of the large-scale field (2.5–2.8 kG at the pole) largely dominates the dipolar component. This large-scale field topology is characteristic of partly convective stars, supporting the conclusion (from evolutionary models) that TW Hya already hosts a radiative core. We also show that TW Hya features a high-latitude photospheric cool spot overlapping with the main magnetic pole (and producing the observed radial velocity fluctuations); this is also where accretion concentrates most of the time, although accretion at lower latitudes is found to occur episodically.

We propose that the relatively rapid rotation of TW Hya (with respect to AA Tau-like cTTSs) directly reflects the weakness of the large-scale dipole, no longer capable of magnetically disrupting the accretion disc up to the corotation radius (at which the Keplerian period equals the stellar rotation period). We therefore conclude that TW Hya is in a phase of rapid spin-up as its large-scale dipole field progressively vanishes.


Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS

Journal keyword(s): techniques: polarimetric - stars: formation - stars: imaging - stars: individual: TW Hya - stars: magnetic field - stars: rotation

Simbad objects: 9

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2019.12.12-19:37:33

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