Magnetic fields and chemical evolution in the disk of the Milky Way

Details Magnetic fields and chemical evolution in the disk of the Milky Way Magnetic fields and chemical evolution in the disk of the Milky Way

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.162...35b&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 162, no. 1, Dec. 1989, p. 35-46.

Astronomy and Astrophysics

Astrophysics

Chemical Evolution, Galactic Evolution, Galactic Structure, Interstellar Magnetic Fields, Milky Way Galaxy, Astronomical Models, Interstellar Gas, Metallicity, Solar Neighborhood, Star Formation, Viscosity

Scientific paper

An alternative noninfall model for the chemical evolution in the solar neighborhood is proposed. The evolution of the disk is divided into two phases. In phase A, the magnetic field and the gas viscosity produced an outward flux of gas, forming and maintaining the ring observed today. This flux balanced the star formation in the ring. The number of stars increased until the beginning of phase B, during which stellar viscosity generated an inward flux of stars toward the inner disk, while the magnetic fields continued supplying gas to the ring. The combination of these two effects brought the ring to a quasi-steady state, with a constant mass of gas and stars which presumably has continued till the present.

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