Physics
Scientific paper
Feb 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981pthph..65..463h&link_type=abstract
Progress of Theoretical Physics, Vol. 65, No. 2, pp. 463-476
Physics
2
Scientific paper
Dynamics of the intracluster gas ejected from galaxies in aspherical clusters has been studied numerically. Assuming the clusters to have oblate mass distributions, we have considered both cases that the clusters are rotating and not rotating.
Calculations show that gas accretion is very much enhanced in the equatorial plane because of the rapid gas expansion around the symmetry axis of a cluster. When the radiative cooling is inefficient, the rotation of a cluster is of no dynamical importance so long as the rotation velocity is smaller than the random velocity of galaxies. In this case the final gas distributions follow approximately the equipotential surfaces of a cluster. On the other hand, when the gas density becomes so large as to force the core to be thermally unstable, the gas mass and its angular momentum in the vicinity of the equatorial plane are concentrated to the core of a cluster. Accordingly, the rotation of a cluster, even if it is much smaller than the random velocity of galaxies, manifests itself as a rapidly rotating, flattened gas disk in the central region of a cluster. The disk contributes to the soft X-ray enhancement.
Hirayama Yoshiharu
Ikeuchi Satoru
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