Magnetocentrifugally driven flows from young stars and disks. 3: Numerical solution of the sub-Alfvenic region

Details Magnetocentrifugally driven flows from young stars and disks. 3: Numerical solution of the sub-Alfvenic region Magnetocentrifugally driven flows from young stars and disks. 3: Numerical solution of the sub-Alfvenic region

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...429..808n&link_type=abstract

The Astrophysical Journal, vol. 429, no. 2, pt. 1, p. 808-825

Computer Science

Numerical Analysis

101

Astronomical Models, Centrifugal Force, Disk Galaxies, Magnetic Fields, Mass Flow, Protostars, Star Formation, Stellar Mass Accretion, T Tauri Stars, Axisymmetric Flow, Bernoulli Theorem, Boundary Conditions, Coordinate Transformations, Magnetohydrodynamic Flow, Numerical Analysis, Steady Flow, Stellar Winds

Scientific paper

We construct steady, axisymmetric, numerical models of the sub-Alfvenic regions of cool winds driven by the X-celerator mechanism. We find that smooth acceleration to speeds of the order of the escape speed accompanied by substantial collimation of the flow can be achieved within the Alfven surface, located characteristically at several stellar radii. We apply the nondimensional results to winds which emerge from the equator of magnetized YSOs rotating at breakup and from circumstellar disks interacting with the magnetospheres of slowly rotating T Tauri stars. Stellar magnetic fields of kilogauss strength can drive wind mass-loss rates of 10-6 solar mass/year from rapidly accreting YSOs and 10-8 solar mass/year from slowly accreting T Tauri stars. The X-celerator mechanism can accelerate winds from these systems to velocities of hundreds of km/sec within a few stellar radii in the case of embedded YSOs and approximately 10 stellar radii in the case of T Tauri stars.

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