where the ultrarelativistic limit of Eq. (18) has been used in the kinetic term. One can immediately see that the electrostatic and gravitational contributions become equal at where the value ξ = 1 / 38 was used for the estimation. The corresponding mass M$_{min}$ = N$_{min}$m$_{B}$ is about 10 13 g, i. e. almost 20 orders of magnitude smaller than the maximum mass of a neutron star. At N$_{B}$ < N$_{min}$ there exists no equilibrium configurations because the kinetic pressure will force the system to expand indefinitely. At N$_{B}$ > N$_{min}$ the negative gravitational contribution exceeds the electrostatic one. The latter becomes completely negligible and can be neglected at baryon numbers ∼ 10 57 characteristic for compact stars. As was first demonstrated by Chandraseckhar [22] and Landau [23], a compact star can be stabilized by the pressure of a degenerate fermion gas alone. From (22) one can see that the balance between kinetic and gravitational energy can be achieved if the total number of baryons is smaller than As follows from this simple calculations, the corresponding maximum mass of a neutron star, M$_{max}$ = N$_{max}$m$_{n}$ is about 3.2 M ⊙ . Numerical calculations within General Relativity [24] for the degenerate noninteracting neutron gas predict somewhat lower maximum mass, M$_{max}$ = 0 . 7 M ⊙ . The repulsive neutron-neutron interaction may increase this value up to 4 M ⊙ (see e.g. ref.[25]). It is easy to see that stars with N$_{min}$ < N$_{B}$ < N$_{max}$ have a stable equilibrium state. Indeed, Eq. (22) shows that in this case W ( R ) > 0 and changes as 1 /R , so that the star should expand to lower densities. But this expansion will terminate at a large enough R , when the neutron gas becomes non-relativistic. As follows from Eq. (18), in this limit the energy per particle is m$_{n}$ + 3 k 2 $_{Fn}$/ 10 m$_{n}$ , i. e. changes as 1 /R 2 at large R . Since the negative gravitational contribution still changes as 1 /R , it wins so that the total energy per baryon approaches m$_{n}$ from below. Therefore a minimum develops in W ( R ). This is famous Landau’s argument presented in ref. [23]. In ref. [25] it was reformulated for the case of General Relativity and for an arbitrary fermion mass. It is clear now that ignoring the kinetic-energy term in Eq. (22), as done in ref. [7], will lead to the erroneous conclusion regarding the star stability. Although the electrostatic and gravitational forces can balance each other at N$_{B}$ = N$_{min}$ , this state corresponds to N$_{min}$ = c$_{3}$ ξ e ( m$_{Pl}$ m$_{B}$ ) 2 ≈ 6 . 26 · 10 36 , (23) N$_{max}$ = ( 3 4 ) 3 / $^{2}$( 9 π 4 ) 1 / $^{2}$( m$_{Pl}$ m$_{n}$ ) 3 ≈ 3 . $^{78}$· 10 57 . (24) 10