TY - JOUR
T1 - He I 1.083 μm emission and absorption in DG Tauri
T2 - Line excitations in the jet, hot wind, and accretion flow
AU - Takami, M.
AU - Chrysostomou, A.
AU - Bailey, J.
AU - Gledhill, T. M.
AU - Tamura, M.
AU - Terada, H.
PY - 2002/3/20
Y1 - 2002/3/20
N2 - We present long-slit spectroscopy and spectroastrometry of He I 1.083 μm emission in the T Tauri star DG Tauri. We identify three components in the He I feature: (1) a blueshifted emission component at ν ≃ -200 km s-1, (2) a bright emission component at zero velocity with a FWZI of ∼500 km s-1, and (3) a blueshifted absorption feature at velocities between -250 and -500 km s-1. The position and velocity of the blueshifted He I emission coincide with a high-velocity component of the [Fe II] 1.257 μm emission, which arises from a jet within an arcsecond of the star. The presence of such a high-excitation line (with an excitation energy of ∼20 eV) within the jet supports the scenario of shock heating. The bright He I component does not show any spatial extension, and it is likely to arise from magnetospheric accretion columns. The blueshifted absorption shows greater velocities than that in Hα, suggesting that these absorption features arise from the accelerating wind close to the star.
AB - We present long-slit spectroscopy and spectroastrometry of He I 1.083 μm emission in the T Tauri star DG Tauri. We identify three components in the He I feature: (1) a blueshifted emission component at ν ≃ -200 km s-1, (2) a bright emission component at zero velocity with a FWZI of ∼500 km s-1, and (3) a blueshifted absorption feature at velocities between -250 and -500 km s-1. The position and velocity of the blueshifted He I emission coincide with a high-velocity component of the [Fe II] 1.257 μm emission, which arises from a jet within an arcsecond of the star. The presence of such a high-excitation line (with an excitation energy of ∼20 eV) within the jet supports the scenario of shock heating. The bright He I component does not show any spatial extension, and it is likely to arise from magnetospheric accretion columns. The blueshifted absorption shows greater velocities than that in Hα, suggesting that these absorption features arise from the accelerating wind close to the star.
KW - Accretion, accretion disks
KW - ISM: jets and outflows
KW - Line: formation
KW - Stars: individual (DG Tauri)
KW - Stars: pre-main-sequence
UR - http://www.scopus.com/inward/record.url?scp=0002853561&partnerID=8YFLogxK
U2 - 10.1086/340277
DO - 10.1086/340277
M3 - Article
AN - SCOPUS:0002853561
VL - 568
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1 II
ER -