Monte Carlo Samples for axion minicluster disruption in the Milky Way

Monte Carlo results for the properties of axion miniclusters in the Milky Way, taking into account pertubations due to stars.<br>The simulations are performed on a grid of semi-major axis a. For each value of a (in pc), we simulate 10^5 AMCs, which are sampled with a log-flat mass function. The labels "PL" and "NFW" specify the internal density profile of the AMCs. For each sample, there are three types of file: 1) AMC_Ninteractions_XXX - the number of expected interactions calculated at the start of the simulation for each AMC. 2) AMC_Ninteractions_true_XXX - the actual number of interactions before the end of the simulation or until the AMC is destroyed.3) AMC_logflat_XXX - individual AMC properties in the Monte Carlo. <br>In files labeled "AMC_logflat_XXX", the columns correspond to:M initial [Msun], R initial [pc], Initial overdensity delta, M final [Msun], R final [pc], Final overdensity delta, eccentricity, orbital inclination psi [radians].<br><br>Files labeled with "circ" assumed an eccentricity of 1 for all orbits (i.e. circular orbits). <br>For more details, see the associated paper "Stellar Disruption of Axion Miniclusters in the Milky Way" (Kavanagh, Edwards, Visinelli, Weniger, 2020) or the associated code (https://github.com/bradkav/axion-miniclusters/).