Crust models

The neutron star crust occupies the low-density outer layers of the star, from the surface down to the crust-core transition density. The crust EOSs are then appended to the core EOS, for instance, by stitching the two together with a spline evaluated in the connection region between the crust and core. For the moment, jester only uses fixed crusts.

Crust files can be provided in .npz file formats and can be loaded and used inside jester via the jesterTOV.eos.crust.Crust class. Check out the API for more information.

In jester, we currently have three very similar crust files derived from the SLy family of EOSs: BPS, DH and SLy, which are shown in the plot below.

(Source code, png, hires.png, pdf)

Pressure (top) and energy density (bottom) as a function of baryon number density for the three built-in crust models. Only the crust region is shown; no core model is appended.

Further resources

• API reference: jesterTOV.eos.crust.Crust