Inner Boundary Velocity Solver

TARDIS operates on a “photospheric” inner boundary approximation. A hard inner boundary in velocity is set from which radiative packets are emitted through the ejecta according to a black-body distribution at a given temperature. Currently, TARDIS can solve for the radiative and inner boundary temperatures as well as dilution factors given a static inner velocity boundary. The precise location of where this inner boundary velocity should be placed is not always obvious and there are a few methods by which one can intelligently select a location based on the properties of the plasma (which are constantly updating over each iteration). This project will aim to update the location of the inner boundary velocity based on a set of options for desired properties of the plasma at each iteration. The options include setting the inner boundary velocity according to a given optical depth over all frequencies (either Planck or Rossland mean opacities) or setting the inner boundary according to a desired value for the dilution factors. The project can be broken down into the following four deliverables: - Estimating the inner velocity value based on target values of optical depth and dilution factor - Integrate the estimation methods into TARDIS base - Write thorough test cases for all the above changes. - Make Jupyter notebooks and tutorials demonstrating the feature. -Thorough documentation of the changes. - Write a blog about the project.