Up to here, we discussed the mass function of planetesimals for the mass range higher than , where the runaway growth takes place. Here we consider the smaller mass range, where the evolution is more complex.
WetherillStewart1993 performed extensive simulations using [a] particle-in-a-box approach, which include[d] both the coagulation and fragmentation, and obtained the mass function. Their result did not depend on the details of the calculation and could be summarized as follows: For the mass range , the power index is close to , in good agreement with our analytical result. For smaller mass, it seems [that] the power index is approximately .
For this low-mass region, we can assume that evolution in their simulation is dominated by the fragmentation process. The formalism of Tanakaetal1996 can also be used for this case. Here, however, the collision rate P has the [the a] power index different from that for the runaway growth region, because the equipartition of the [delete ``the''] energy is not established and gravitational focusing is not effective. In this case, we have and therefore . This result is in fair agreement with the numerical result of WetherillStewart1993, for the intermediate mass range (). For even smaller mass[es], they obtained [a] somewhat shallower slope. This is the natural result of the positive dependence of the velocity dispersion to [to on] the mass due to strong gas drag.
Using [an] exact analytic treatment, we obtained the power-law mass distribution of planetesimals which has been found in numerical simulations of the [delete ``the''] runaway growth. The mechanism through which the power-law distribution is realized is directly related to the occurrence of the [delete ``the''] runaway growth, where heavier planetesimals grow faster than lighter planetesimals.
Our treatment of the [delete ``the''] runaway growth is different from those in previous theoretical works (see, , Ohtsuki and Ida 1990, Ida and Makino 1992a, 1992b), where [the] growth rate were [were was] obtained for different planetesimals in the background distribution of single-mass planetesimals. In those analyses, the difference in the growth rate[s] can come only from the difference in the mass of the planetesimals under consideration. In other words, previous works dealt with the growth of the small perturbation of the mass from the uniform distribution (linear stability analysis).
In the present work, we investigated the evolution of [the] mass distribution function which is far from uniform, taking into account the non-uniformity of the background distribution as well. As a result, we were able to derive the stationary distribution, which is consistent with the result of numerical experiments.
Our result suggests that the power-law mass distribution of planetesimals is a universal law which is realized in the early stage of the [delete ``the''] runaway growth. Since the evolution of the mass function in the late runaway stage is quite slow [,], we can conclude that the distribution of the mass of planetesimals is described with [is described with follows] this power law for most of the planet formation period. The mass distribution for smaller masses (less than ) is expressed by a different power law, since in this regime the [delete ``the''] energy equipartition is not established.