  Properties of neutron star are investigated by an available relativistic $ab~
initio$ method, i.e., the relativistic Brueckner-Hartree-Fock (RBHF) model,
with the latest high-precision relativistic charge-dependent potentials,
pvCD-Bonn A, B, C. The neutron star matter is solved within the beta
equilibrium and charge neutrality conditions in the framework of RBHF model.
Comparing to the conventional treatment, where the chemical potential of lepton
was approximately represented by the symmetry energy of nuclear matter, the
equation of state (EOS) of neutron star matter in the present self-consistent
calculation with pvCD-Bonn B has striking difference above the baryon number
density $n_b=0.55$ fm$^{-3}$. However, these differences influence the global
properties of neutron star only about $1\%\sim2\%$. Then, three two-body
potentials pvCD-Bonn A, B, C, with different tensor components, are
systematically applied in RBHF model to calculate the properties of neutron
star. It is found that the maximum masses of neutron star are around
$2.21\sim2.30M_\odot$ and the corresponding radii are $R =11.18\sim11.72$ km.
The radii of $1.4M_\odot$ neutron star are predicated as $R_{1.4} =
12.34\sim12.91$ km and their dimensionless tidal deformabilities are
$\Lambda_{1.4} = 485\sim 626$. Furthermore, the direct URCA process in neutron
star cooling will happen from $n_b=0.414\sim0.530$ fm$^{-3}$ with the proton
fractions, $Y_p=0.136\sim0.138$. All of the results obtained from RBHF model
only with two-body pvCD-Bonn potentials completely satisfy various constraints
from recent astronomical observations of massive neutron stars, gravitational
wave detection (GW 170817), and mass-radius simultaneous measurement (NICER).
