Date post: | 20-Dec-2015 |
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Magnetic Field Detection in CTTSMagnetic 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).
Accreting Field ExtrapolationsAccreting Field Extrapolations
(Gregory et al. 2004, in preparation)
• LQ Hya surface
map.
• Potential field
extrapolation with
source surface.
• Isothermal corona
in hydrostatic
equilibrium.
Accreting Field ExtrapolationsAccreting Field Extrapolations
(Gregory et al. 2004, in preparation)
• AB Dor surface
map.
• Potential field
extrapolation with
source surface.
• Isothermal corona
in hydrostatic
equilibrium.
Future WorkFuture 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.