  We solve the Tolman-Oppenheimer-Volkoff equation using an equation of state
(EoS) calculated in holographic QCD. The aim is to use compact astrophysical
objects like neutron stars as an indicator to test holographic equations of
state. We first try an EoS from a dense D4/D8/\textoverline {D8} model. In this
case, however, we could not find a stable compact star, a star satisfying
pressure-zero condition with a radius $R$, $p(R)=0$, within a reasonable value
of the radius. This means that the EoS from the D4/D8/\textoverline {D8} model
may not support any stable compact stars or may support one whose radius is
very large. This might be due to a deficit of attractive force from a scalar
field or two-pion exchange in the D4/D8/\textoverline {D8} model. Then, we
consider D4/D6 type models with different number of quark flavors, $N_f=1,2,3$.
Though the mass and radius of a holographic star is larger than those of normal
neutron stars, the D4/D6 type EoS renders a stable compact star.

High Energy Physics - Phenomenology;High Energy Astrophysical Phenomena;Nuclear Theory