Relativistic dynamics of stars near a supermassive black hole

<p>This data was first presented in `Relativistic dynamics of stars near a supermassive black hole&rsquo; (Hamers et al. 2014, MNRAS 443, 1; http://mnras.oxfordjournals.org/content/443/1/355; doi: 10.1093/mnras/stu1126). It includes the first- and second-order diffusion coefficients (DFCs) from the S-star N-body simulations (cf. Section 5.1 from the paper) as a function of the angular-momentum variable \ell = \sqrt{1-e^2}, binned with respect to the semimajor axis (cf. Section 5.4 from the paper).</p> <p>Description of the comma-separated txt files:<br /> `a_bins.txt&rsquo; - the semimajor axis bins. Semimajor axes are given in units of mpc (milliparsec). First column: the index of the bin; second column: the lower bin value; third column: the upper bin value; fourth column: the mean value.<br /> `D12_l_index_a_bin_i.txt&rsquo; - the DFCs for the different semimajor axis bins as a function of \ell (i is the bin index). First column: the value of \ell; second column: the first-order DFC, in units of 1/Myr; third column: the second-order DFC, in units of 1/Myr.</p> <p>Adrian Hamers, 22 April 2016</p>