Computer Science
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..14e..30l&link_type=abstract
Modelling Dense Stellar Systems, 26th meeting of the IAU, Joint Discussion 14, 22-23 August 2006, Prague, Czech Republic, JD14,
Computer Science
Scientific paper
We present N-body simulations of star clusters containing initial mass function in the galaxy to study effects of tidal field systematically on the properties of outer parts of globular clusters. For simplicity, we have employed only spherical components (bulge and halo) of the Galaxy. Total number of stars in our simulations was about 20,000. All simulations were done for several orbital periods in order to understand the development of the tidal tails. In our scaled down models, the relaxation time is sufficiently short to show the mass segregation effect and core collapse. The directions of tidal tails are determined by the orbits and locations of the clusters. We find that the length of tidal tails increases toward the apogalacticon and decreases toward the perigalacticon. This anti-correlation between the strength of the tidal field and the length of the tail is caused by the fact that the time scale for the stars to respond to the potential is similar to the orbital time scale of the cluster. When the length of tidal tails decreases some of the stars in the tidal tails are recaptured by the host cluster. From the investigation of velocity anisotropy of the model clusters, we find that in the early stages of globular cluster evolution the clusters have radial anisotropy in the outermost parts, while clusters are nearly isotropic in the central region. The radial anisotropy decreases with time. We also extend out work to the initially rotating clusters. For clusters in retrograde orbit, we find that the sense of internal rotation changes from the inner to outer parts: while the inner part remembers the initial sense of rotation for a long time, the direction of the rotation of the outer parts is determined by the orbital direction.
Ahn I. S.
Lee Han-Koo
Lee Michael H.
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