This repository provides two Jupyter notebooks and accompanying files to recreate the results and plots of Graber et al. (2018). Please cite Graber et al. (2018) as well as 
The Jupyter notebook rapid_crust_coupling.ipynb contains code to integrate the TOV equations for a specific neutron star crust model and calculate the mutual friction coefficients as a function of cylindrical radius and relative mass fraction. It subsequently allows numerical integration of a simple three-component neutron star toy model, providing the time evolution of the angular velocities, to determine the characteristic shape of the glitch rise of a Vela-like pulsar. A preliminary comparison between these theoretical predictions and the first single-pulse radio observations by Palfreyman et al. (2018) as discussed in Section 5 of Graber et al. (2018) is provided in the Jupyter notebook data_comparison.ipynb.
The file microscopic_parameters.txt contains the microscopic parameters for the inner crust as given in Table 1 of Graber et al. (2018). Moreover, 41586_2018_1_MOESM1_ESM.csv consists of the data for the observed glitch provided by Palfreyman et al. (2018), whereas the files model_residuals_Bcore5e-5.txt and model_residuals_Bcore_comparison.txt contain the corresponding predictions as obtained from theoretical models.
We also provide the environment file that has been used to create our results. It can be installed by running conda env create -f environment.yaml
and has been tested under Linux, Mac OS and Microsoft. Please contact the author if you have any problems.
This project is licensed under the MIT License - see the LICENSE.md file for details.