Evolution of Globular Clusters

Astronomy 626: Spring 1995

The evolution of globular clusters is complicated by galactic tidal forces, mass loss due to stellar evolution, and dissipative stellar encounters. However, some globular clusters have luminosity profiles which rise to the innermost point measured; these systems have probably undergone core collapse.

External Influences

Tidal radii

                  m   1/3
(1)     r_t = D (---)    .
                 3 M

Michie-King models

                     -beta(E - E_t)
(2)     f(E)  =  K (e               - 1) ,    if  E < E_t ,

              =            0             ,    otherwise .

Stellar Evolution

Rates & endpoints

Expansion & disruption

Dissipative Effects

References

• Chernoff, D.F. & Weinberg, M.D. 1990, Ap. J. 351, 121.
• Cohn, H. & Hut, P. 1984, Ap. J. 277, L45.
• Djorgovski, S. & King, I.R. 1984, Ap. J. 277, L49.
• Elson, R., Hut, P., & Inagaki, S. 1987, Ann. Rev. Astr. Ap. 25, 565.
• King, I.R. 1966, A. J. 61, 64.

Last modified: May 3, 1995