List of Figures

View Image Figure 1:
Globular cluster distribution about the galaxy. Positions are from Harris [95] and are plotted as black circles on top of the COBE FIRAS 2.2 micron map of the Galaxy using a Mollweide projection. Figure taken from Brian Chaboyer’s website [32].
View Image Figure 2:
Hubble Space Telescope photograph of the dense globular cluster M80 (NGC 6093).
View Image Figure 3:
Color–magnitude diagram for M80. Figure taken from the catalog of 52 globular clusters [203]. The entire catalog is available at the Padova Globular Cluster Group website [231].
View Image Figure 4:
Lagrange radii indicating the evolution of a Plummer model globular cluster for an N-body simulation and a Monte Carlo simulation. The radii correspond to radii containing 0.35, 1, 3.5, 5, 7, 10, 14, 20, 30, 40, 50, 60, 70, and 80% of the total mass. Figure taken from Joshi et al. [126].
View Image Figure 5:
CMD of M3 from the Hubble Space Telescope WFPC2. Note the stars above and to the left of the turn-off. These are the blue stragglers. Figure taken from Zhao and Bailyn [246].
View Image Figure 6:
Cross section of equipotential surfaces in the orbital plane of a binary with q = 0.4. The values of the potential surfaces are 5.0, 3.9075, 3.8, 3.559, 3.2, 3.0, and 2.8. The units have been normalized to the orbital separation, so a = 1.
View Image Figure 7:
Evolution of the radius for a 10 M ⊙ star with Z = 0.001. Figure taken from Pfahl et al. [177].
View Image Figure 8:
Example of a binary-field star exchange interaction. The binary comes in from the right (red-white), while the field star (green) enters from the left. After a complicated interaction, the white star is ejected and the newly formed red-green binary is in a more tightly bound orbit. Figure taken from McMillan [154].
View Image Figure 9:
Results of the Monte Carlo simulation of NS–WD binary generation and evolution in 47 Tuc. Each small dot represents a binary system. The circles and error bars are the 10 binary pulsars in 47 Tuc with well measured orbits. Systems in A have evolved through mass transfer from the white dwarf to the neutron star. Systems in B have not yet evolved through gravitational radiation to begin RLOF from the white dwarf to the neutron star. Systems in C will not undergo a common envelope phase. Figure taken from Rasio et al. [198].
View Image Figure 10:
Binary period distributions from the Monte Carlo simulation of binary fraction evolution in 47 Tuc. The bottom panel indicates the period distribution for binaries containing at least one white dwarf. Nb is the total number of binaries and Nb,p is the number of binaries per bin. Figure taken from Ivanova et al. [120].