Example use-case: Orbit integration and supernova kicks

As stars form in larger systems like galaxies, they also move through these systems over time.

Whether we can connect such an evolution with SSPC depends on whether the sysstem is collisionless and does not involve dynamical scatterings.

In collissionless systems, the position and velocity of a star system (or its centre of mass) is dictated by the collisionless boltzmann equation. On top of this motion, massive stars can also experience kicks due to supernovae.

This notebook intends to show how to set up a post-convolution method that evolves te position and velocity of a (binary) star system under the influence of the gravitational field of a galaxy, as well as additional supernova kicks. We will use AGAMA (Vasiliev 2019) for this, but other codes could be used too.

TODO: standard setup TODO: generate and load data with kicks TODO: design a post-convolution code

The post-convolution function should do the following things:

• sample systems based on the convolution results

• set up an agama potential of choice

• assign positions and velocities to the systems, as well as inclinations for binary systems

• integrate the systems forward in time until current day

  • when a supernova kick occurs in between the convolution bin time and current day: apply supernova kick

The input data should contain the following:

• systems forming compact objects

• related supernova information:

  • kick direction

  • kick velocity

  • (if binary) companion kick direction

  • (if binary) companion kick velocity

  • supernova number (can be two)

  • whether the supernova occurs if the system is bound