The solid line that illustrates the evolutionary path of a star like the Sun in Figure 59.4 is a bit deceptive. It gives the impression that we are as likely to see stars like the Sun in their protostar phase as in their main-sequence phase. However a star moves through some phases rapidly and others much more slowly. If instead of a line you put down one point for every 10 million years, you would get a better idea of where you would be likely to see stars like the Sun in the H-R diagram. Lightly sketch or trace the Sun's evolutionary path in an H-R diagram and then use the following times to estimate how many dots to put down in each portion of the Sun's evolutionary path: protostar phase $\sim 20$ million years (Myr); main-sequence phase $\sim 10,000 \mathrm{Myr}$ first red giant phase $\sim 1000$ Myr; yellow giant phase $\sim 100$ Myr; second red giant phase $\sim 10$ Myr; planetary nebula phase $0.01 \mathrm{Myr} ;$ white dwarf phase $\sim 3000$ Myr. (The star remains a white dwarf beyond this time, but fades from visibility.)