Steiner (2012) Data Files
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:
Back to Andrew W. Steiner at
the University of Tennessee.