Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...433...39e&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 433, no. 1, p. 39-47
Astronomy and Astrophysics
Astrophysics
88
Galactic Structure, Gravitation Theory, Gravitational Collapse, Interstellar Gas, Magnetic Clouds, Molecular Clouds, Spiral Galaxies, Star Formation, Astronomical Models, Interstellar Magnetic Fields, Mathematical Models, Radial Distribution
Scientific paper
The dispersion relations for radial and azimuthal gravitational instabilities in a magnetic gas that flows through a spiral density wave are derived considering the time-dependent flow and shear fields in the linear wave. The results are approximately the same as the dispersion relations without the spiral wave except for the substitution of local values for the density, magnetic field strength, and epicyclic frequency. The instability leads to the formation of 107 solar mass cloud complexes with a characteristic spacing of approximately 3 times the arm width. Spiral arms can trigger an excess of star formation if the arm density exceeds several times the average critical value at that radius and if (G)(mu)/(c sq) greater than 1 for mass per unit length mu along the arm and velocity dispersion c.
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