  We investigate the magneto--elastic equilibrium of a neutron star crust and
magnetic energy stored by the elastic force. The solenoidal motion driven by
the Lorentz force can be controlled by the magnetic elastic force, so that
conditions for the magnetic field strength and geometry are less restrictive.
For equilibrium models, the minor solenoidal part of the magnetic force is
balanced by a weak elastic force because the irrotational part is balanced by
the dominant gravity and pressure forces. Therefore, a strong magnetic field
may be confined in the interior, regardless of poloidal or toroidal components.
We numerically calculated axially symmetric models with the maximum
shear--strain, and found that a magnetic energy $> 10^{46}$ erg can be stored
in the crust, even for a normal surface dipole-field-strength ($<10^{13}$ G).
The magnetic energy much exceeds the elastic energy ($ 10^{44} -10^{45}$ erg).
The shear--stress spatial distribution revealed that the elastic structure is
likely to break down near the surface. In particular, the critical position is
highly localized at a depth less than 100 m from the surface.
