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README.md

Summerstudent project

Git for summerstudent project on evolution of open cluster (see project description)

A manual to run the code and get output in correct format is present: nbody6_quick_guide.md.

TODO list:

Practicalities

  • Get nbody6 working and get to know the code
    • Make appointment with max and go through things
  • Make it fairly easy for the student to work with nbody6
    • make output scripts
    • Create environment to run things on. i.e. go to IT
  • Ask someone to send us a couple of review papers on clusters
  • Write up a more solid form of the project description
  • Stay in contact with Mark and Fabio, keep them in the loop of any further advice. Also discuss with them semi regularly about the topic.
  • Create quickstart manual for us
  • Try out mcluster for the setup of Nbody simulation settings. They have a nice manual
  • Fix script for mcluster to put everything in a nice place with the logs
  • Finish the python config generator.

Scientific

  • Decide upon the following scientific things:
    • Total mass: What range of cluster masses/Total number of stars will we decide to evolve?
    • Density profile: What will be the density profile that is the most sensible? See paper of Douglas and Heggie for inspiration
    • Tidal field: Vary between no tidal field and tidal field? Think about this
    • Binary fraction: Binary fraction for stars, and will we do a uniform one or mass dependant?
    • Eccentricity distribution: Thermal is fine, but flat is also okay i think.
    • Period distribution: Sana 2012 if possible.
    • Initial mass function: Lets decide to start by using the standard kroupa for now, no reason to do so otherwise, however choosing single mass is maybe good as a reference to other work.
      • Mass limits: Decide which mass limits to take. Is 100 solarmass enough?
    • Mass Segregation: I think no initial segregation, because we want to see, with an initial cluster, how the segregation occurs. But i am not sure if forming clusters have any segregation at all?
    • Fractality: This is to simulate the imperfectness of the spatial distribution of stars at formation. I wonder how this can affect the outcomes.
    • Stellar evolution settings:
      • Use pre-evolved setting with cluster, might be fun to test out the paper via a shortcut