Bipolar hydromagnetic winds from disks around protostellar objects

Details Bipolar hydromagnetic winds from disks around protostellar objects Bipolar hydromagnetic winds from disks around protostellar objects

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...301..571p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 301, Feb. 15, 1986, p. 571-586. Research supported by the Johns Hopkins Uni

Physics

304

Magnetohydrodynamics, Pre-Main Sequence Stars, Protostars, Stellar Evolution, Stellar Winds, Acceleration (Physics), Galactic Nuclei, Magnetic Field Configurations, Molecular Clouds, Momentum Transfer, T Tauri Stars, Torque

Scientific paper

The bipolar outflows associated with protostars are modeled as two-component, hydromagnetic winds which originate in the envelopes of rotating, magnetized molecular disks. The authors show that the torques exerted upon disks by centrifugally driven winds can account for both the observed linear momentum and energy transport rates associated with the molecular outflows. The prediction is that the luminosity associated with protostellar objects during the molecular outflow epoch is due to accretion from these disks. These outflows can solve the angular-momentum problem of star formation and drive accretion onto the protostellar cores. The molecular outflow produces a magnetohydrodynamic shock as it collides with ambient molecular cloud gas with characteristic H2 emission produced in the preshock region. Calculations are presented for the masses, rotation rates, and densities, and outflow characteristics for disks and their outflows, for the sources HH 7-11 (SVS 13), Orion-KL (IRc2), L1551 (IRS 5), and B335.

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