Intro

1
Accretion Channeling in CTTS
Scott Gregory, Moira Jardine
2
Classical T Tauri Stars (CTTS)
(Goodson et al. 1997)
3
Magnetic Field Detection in CTTS

• Surface fields of 1-3 kG detected from
• Zeeman broadened spectral lines
• (e.g. Johns-Krull et al. 1999).
• Circularly polarised lines
• Increased line equivalent widths
• (e.g. Guenther et al. 1999).
• Electron-cyclotron maser emission
• (Smith et al. 2003).

4
Accreting Field Extrapolations

• LQ Hya surface map.
• Potential field extrapolation with source
  surface.
• Isothermal corona in hydrostatic equilibrium.

(Gregory et al. 2004, in preparation)
5
Accreting Field Extrapolations

• AB Dor surface map.
• Potential field extrapolation with source
  surface.
• Isothermal corona in hydrostatic equilibrium.

(Gregory et al. 2004, in preparation)
6
Accretion Footpoints
Latitude
Longitude
Latitude
Longitude
7
Future Work X-ray Emission
8
Future Work X-ray Emission
9
Future Work

• ESPaDOnS (Echelle SpectroPolarimetric Device for
  the Observation of Stars at CFHT)
• Observations of DF Tau and BP Tau (plus V410 Tau
  and V830 Tau) in 2005.
• (Petit, Donati the ESPaDOnS project team
  2004)
• Magnetospheric accretion models with potential
  field extrapolations.