Data for "Instability in supernova fallback disks and its effect on the formation of ultra long period pulsars"

This dataset gives the monte-carlo simulated data used in its related article, where the folder names denote the corresponding models:

mc_r300_ref: Using T=300K as the criteria for the disk neutralization (R_neu2), and partial instability; 

mc_r300_glo: Using T=300K as the criteria for the disk neutralization (R_neu2), and global instability;

mc_r6500_ref: Using T=6500K as the criteria for the disk neutralization (R_neu1), and partial instability;

mc_r6500_glo: Using T=6500K as the criteria for the disk neutralization (R_neu1), and global instability.

Each folder contains four ".data" files, corresponding to the simulated data for different time points: 1 kyr, 10 kyr, 100 kyr and 1 Myr. These files can be easily read and used to replicate our MC results.

Moreover, reproducing our results may require the following data columns from the files:

"ids": "=1" represents the disk can form, while "=0" not;

"da": "=1" represents the disk can exist, while "=0" not;

"mdisk0": the initial mass (unit: solar mass) of the fallback disk;

"rf0": the initial outer radius (unit: Schwartzschild radius) of the fallback disk;

"alpha0": the initial disk inclination angle of the fallback disk;

"p0": the initial spin period of the neutron star;

"bns0": the initial magnetic field strength of the neutron star;

"chi0": the initial magnetic inclination angle of the neutron star;

"*_f": the values at the specific time point (i.e. 1 kyr, 10 kyr, 100 kyr or 1 Myr);

"omegadot": the time derivative of spin angular velocity;

"rin", "rco", and "rlc": the inner radius, the corotation radius and the light cylinder radius;

"n1", "n2" and "n3": the accertion torque, the torque caused by the magnetic-disk interaction and the dipole radiation torque.

Overall, this data repository is intended to facilitate the reproduction of the results related to the Monte Carlo simulations presented in the article: Instability in supernova fallback disks and its effect on the formation of ultra long period pulsars. If you encounter any issues while using the data, please feel free to contact us at this email: [e-mail]