Statistics – Computation
Scientific paper
Nov 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...225..507d&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 225, no. 2, Nov. 1989, p. 507-516.
Statistics
Computation
7
Computational Astrophysics, Interstellar Magnetic Fields, Interstellar Matter, Molecular Clouds, Star Formation, Bessel Functions, Density Distribution, Magnetic Field Configurations, Velocity Distribution
Scientific paper
The collapse of a magnetic rotating gas cloud is followed up to twice the free-fall time by numerical calculations. The initial magnetic field of 3 microG and the axis of rotation are inclined relative to each other at an angle of 45 deg. The mass of the cloud is 10,000 solar mass, the radius is 6.5 x 10 to the 19th cm and hence, the density is 1.73 x 10 to the -23rd g/cu cm. The rotational velocity is set to the galactic angular velocity of 10 to the -15th/sec. The temperature of 100 K is kept fixed throughout the whole calculation. The temporal evolution exhibits oscillatory motions over a wide range of scales. The efficiency of magnetic braking lies between that the perpendicular and the aligned cases. The exerted magnetic torques rotate the total angular momentum vector toward the field direction. Analytical estimates for braking time scales and for temporal evolution of the total angular momentum vector of rotating self-gravitating interstellar clouds are derived for different angles of inclination between the magnetic field and the axis of rotation. These results are compared with the detailed three-dimensional numerical calculations.
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