Day 50

Wednesday.  SCAMP going slower than expected, but hope to get some good info from Gary today.  I don't want to slack off on day 50!


1107.4095
Long-term evolution of massive black hole binaries.  IV. Mergers of galaxies with collisionally relaxed nuclei
Gualandris, Merritt


N-body simulation of two galaxies with collisionally-relaxed (MBH+star) cores, to study the distribution of "stellar-mass BHs" (?) after the merger.  There are 4 mass groups representing old stellar populations.  Merger assumption: 1:3 mass ratio, two different orbits.  During merger, initial mass distribution erased, large cores are carved out in the stellar distribution (several times the radius of influence of the massive BH).  Follow for 3 central relaxation times after coalescence of the massive binary: standard and top-heavy mass functions are considered.  Cores persist; the distribution of stellar-mass BHs evolves against this fixed BG.  After 3 relaxation times, it still looks different from the relaxed, multi-mass models often assumed to describe distribution of stars and stellar remnants near massive BH; e.g. density of stellar BH much smaller in the models.  


* EMRI problem:  "Extreme mass ratio inspiral"
* Bahcall-Wolf cusps:  density cusp around a massive object (BH)


* I want to know if the consider DM and stellar mass separately (both are non-interacting particles); what they probably do is assign certain DM particles as stars (and paint them in 4 different colors, depending on their initial position).