Right panel Sample Clauses

Right panel. Using Eqn. (2.6) and the (M ) relation for axion stars, we calculate the gravitational wave frequencies for axion star and BH equal mass binary mergers. Figure 2.10: Peaks of the toy model density as Fig. 2.9 with fa = 0.5 Mpl (left panel) and fa = 0.1 Mpl (right panel). Note that as fa dips below the triple point [114], a dispersal gap appears between the formation of black holes and axion stars. The peak statistics are determined by thresholding the field, and are classified using a two pass connected component clustering algorithm, see Sec. 2.4.3. We par- tition the distribution for M˜y(fa) according to the critical masses Mdisp. and MBH in the phase diagram [114]. In our numerical simulations, due to the construction with periodic boundary conditions and an isolated fluctuation, fluctuations of all amplitudes leading to axion stars with radius smaller than the box size will even- tually collapse under self-gravity. Thus we cannot determine the critical threshold for axion star collapse. However, we are only interested phenomenologically in the densest, and thus most massive stars, and so we threshold our field for a mini- mum compactness of the final axion star assuming that at least these most compact objects successfully collapse.