Collisions between rotating interstellar clouds

Details Collisions between rotating interstellar clouds Collisions between rotating interstellar clouds

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.232..565l&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 232, June 1, 1988, p. 565-614.

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Interstellar Matter, Molecular Clouds, Molecular Collisions, Rotating Matter, Spin-Orbit Interactions, Supersonic Speed, Angular Velocity, Computational Astrophysics, Kinetic Energy

Scientific paper

The paper presents three-dimensional numerical hydrodynamic simulations of collisions between rotating interstellar clouds. The results show that rotation can significantly extend the lifetimes of the resulting structures when compared to comparable cases without rotation. In many cases, it is found that rapidly rotating bars form, and in some cases these can form quasi-equilibrium structures which reexpand very slowly, surviving for many free-fall times. The calculations also show the importance of spin-orbit interactions in the case of off-center collisions. It is found that, despite rapid dissipation in the collisions, the kinetic energy of each interacting pair of clouds often increases, thus providing a possible way of maintaining supersonic motions in interstellar cloud complexes. The resultant collapsing structures often assume a nearly solid-body rotation law in the inner regions, and a Keplerian profile beyond this. This latter fact indicates that rotational support is more important in these structures than is thermal support.

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