Physics
Scientific paper
Jun 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...409..748g&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 409, no. 2, p. 748-761.
Physics
35
Accretion Disks, Emission Spectra, Pre-Main Sequence Stars, Stellar Models, Stellar Physics, Stellar Winds, Color-Color Diagram, Forbidden Bands, Line Spectra, Shock Waves, T Tauri Stars
Scientific paper
We present a model for the origin of blueshifted, optical forbidden line emission and jets in young stellar objects based on generic properties of hydromagnetic disk winds. Magnetic stresses recollimate hydromagnetic disk winds to magnetic focal regions under very general conditions. We demonstrate that conditions in MHD shocks at these points account for the observed emission. We find that for fiducial accretion rates of 10 exp -7 solar masses/yr and magnetic fields at the inner edge of the disk of about 10 exp 12 cm, gas accelerated from the innermost parts of a Keplerian accretion disk focuses into regions equal to or greater than 0.4 AU in radius that lie about 16 AU above and below the disk. The shocked gas density ranges from 10 exp 4 to 10 exp 8/cu cm where the latter occurs in the innermost part of the flow and shock. Shocked gas speeds range up to 250 km/s (going from the outer part of the shock at about 2 AU, to the innermost region) under these conditions. The magnetic field is moderately amplified in the shock and diverges from the flow axis in the postshock flow. It is this feature of MHD shock that produces an expanding cone of shocked gas. The opening angle of the postshock gas with respect to the flow axis is 40 deg, and this accounts for the double-peaked character of the line profiles. Our model also predicts that the slower velocity component is associated with shocked gas of lower density than that associated with the higher velocity component.
Gomez de Castro Ana Ines
Pudritz Ralph E.
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