3D models for self-gravitating, rotating magnetic interstellar clouds

Details 3D models for self-gravitating, rotating magnetic interstellar clouds 3D models for self-gravitating, rotating magnetic interstellar clouds

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...114..151d&link_type=abstract

Astronomy and Astrophysics, vol. 114, no. 1, Oct. 1982, p. 151-164.

Astronomy and Astrophysics

Astrophysics

56

Astronomical Models, Gravitational Collapse, Interstellar Gas, Interstellar Magnetic Fields, Magnetic Clouds, Molecular Clouds, Rotating Fluids, Three Dimensional Models, Angular Momentum, Magnetohydrodynamics, Stellar Evolution

Scientific paper

Results of 3D numerical calculations on the dynamics of rotating, magnetized, and self-gravitating gas clouds are presented. The magnetic field is treated as frozen in the matter, and two cases where a homogeneous field of 3 microG is either perpendicular to or aligned with the axis of rotation are considered. Starting with an interstellar cloud of 10,000 solar masses with an initial density of 1.73 x 10 to the -23rd g/cu cm, a uniform galactic angular velocity (10 to the -15th/sec) is assumed. This isothermal cloud (T equals 100 K) with a radius of 6.5 x 10 to the 16th cm is embedded in a tenuous medium of 1.73 x 10 to the -24th g/cu cm at rest. The calculations were performed on a 3D Cartesian hierarchical grid. Results show that for a cloud with these parameters, magnetic braking can remove the bulk of the cloud's angular momentum in times that are short compared with the free-fall time. The magnetic field can also prevent the major part of a cloud from collapse and favors the formation of highly nonhomologous, bar-like structures. It is shown that the initial structure of the magnetic field is strongly modified during the evolution. While numerical diffusion is responsible for changes in the field topology, similar effects may occur when physical diffusion is explicitly included. Diffusion can cause turbulence in interstellar clouds and defines the final amount of angular momentum of the remaining, gravitationally bound fragments.

Affiliated with

Also associated with

No associations

Rating

3D models for self-gravitating, rotating magnetic interstellar clouds does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with 3D models for self-gravitating, rotating magnetic interstellar clouds, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and 3D models for self-gravitating, rotating magnetic interstellar clouds will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1028455