## Format

The HDF5 files contain the full data sets and the text files contain the same information (except at a lower precision). The HDF5 format is relatively straightforward, except that the column names and units are each stored as two sets of integer arrays. One array specifies the size of each string representing the column name (or unit) and the other specifies the ASCII integers for each character. (This format allows me to use HDF5 chunking and ensure that columns can be added to the table easily.)

## Cold crust

The data files are organized into tables which contain the following columns

• nb: baryon number density
• rho: rest mass density
• N: neutron number (neutrons inside nucleus)
• Z: proton number
• nn: neutron number density (neutrons outside nucleus)
• ede: energy density from electrons
• ne: electron number density
• fr: free energy density (equal to internal energy density since $T=0$ )
• nnuc: number of nuclei per unit volume
• chi: volume fraction occupied by nuclei
• nnL: number density of neutrons inside nuclei
• npL: number density of protons inside nuclei
• pr: pressure
• Rws: size of the Wigner-Seitz cell
• Rn: the neutron RMS radius for nuclei
• Rp: the proton RMS radius for nuclei
• Ncell: the number of neutrons outside nuclei
• cs2: speed of sound
• fcs2: speed of sound at fixed electron fraction
The files are:

## Accreted crust

The data files are organized into tables which contain the following columns

• nb: baryon number density
• rho: rest mass density
• Ye: electron fraction
• fr: free energy density
• Z: average atomic number
• A: average mass number
• Q: impurity parameter
• a: average inter-ionic spacing
• pr: pressure
The files are:

## Core

The data files are organized into tables which contain the following columns exactly as done in the o2scl::nstar_cold class documented here.

The files are:

## TOV profiles

Profiles for a $1.4~\mathrm{M}_{\odot}$ neutron star

The files are: