 Without proclaiming the laws of nature time asymmetric, there is no way to eliminate as impossible transitions  (2)  in favor of  (1).  Nevertheless, appealing to temporally asymmetric boundary conditions allows us to describe a world wherein  (1)  but not  (2)  occur. A cosmological hypothesis claiming that in the very distant past entropy was much lower will work. Boltzmann, as well as many of this century’s greatest scientists, e.g., Einstein, Richard Feynman, and Erwin Schroedinger, saw that this hypothesis is necessary given our (mostly) time asymmetric laws. (Boltzmann, however, explained this low-entropy condition by treating the observable universe as a natural statistical fluctuation away from equilibrium in a vastly larger universe.) Earlier states do not have higher entropy than present states because we make the cosmological posit that the universe began in an extremely tiny section of its available phase space. Albert (2000) calls this the “Past Hypothesis” and argues that it solves both this problem of the direction of time and also the one to be discussed below. Note that classical mechanics is also compatible with a “Future Hypothesis”: the claim that entropy is very low in the distant future. The restriction to “distant” is needed, for if the near future were of low-entropy, we would not expect the thermodynamic behavior that we see—see Cocke 1967, Price 1996, and Schulman 1997 for discussion of two-time boundary conditions.