Astronomy and Astrophysics – Astronomy
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...462..439k&link_type=abstract
Astrophysical Journal v.462, p.439
Astronomy and Astrophysics
Astronomy
66
Accretion, Accretion Disks, Infrared: Stars, Stars: Magnetic Fields, Stars: Pre-Main-Sequence
Scientific paper
We describe a magnetic accretion disk model for the infrared colors of T Tauri stars in the Taurus-Auriga molecular cloud. In this model, the stellar magnetic field truncates the disk several stellar radii above the stellar photosphere; material then flows along magnetic field lines and forms a bright ring at which the accretion stream impacts the star. The model successfully reproduces the observations for reasonable values of the magnetic field strength, 100-500 G; the stellar rotational period, 4-10 days; and the mass accretion rate, 10-8 to 10-6 Msun yr-1. The truncation radius, R0, lies well inside the corotation radius, Rc. We estimate R0/Rc ≍ 0.6-0.8 for classical T Tauri stars in our sample. This result constrains models for the rotational evolution and bipolar outflows of pre-main-sequence stars.
Magnetic disk models make several testable predictions. The near-IR colors should correlate with the stellar magnetic field and the rotational period. The magnitude of the near-IR veiling should correlate strongly with the stellar rotational period. Strong CO emission or absorption features should be present only in stars with high accretion rates. Observations also discriminate between various types of magnetic disk geometries if intrinsic stellar parameters, such as the stellar radius and magnetic field strength, are well known.
Hartmann Lee
Kenyon Scott. J.
Yi Insu
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