  Background: The equations of state (EoSs) which determine the properties of
neutron stars (NSs) are often characterized by the iso-scalar and iso-vector
nuclear matter parameters (NMPs). Recent attempts to relate the radius and
tidal deformability of a NS to the individual NMPs have been inconclusive.
These properties display strong correlations with the pressure of NS matter
which depends on several NMPs. The knowledge of minimal NMPs that determine the
NS properties will be necessary to address any connection between NS properties
(e.g., tidal deformability) and that of finite nuclei.
  Purpose: To identify the important NMPs required to describe the tidal
deformability of neutron star for astrophysically relevant range of their
gravitational masses (1.2 -- 1.8 M$_\odot$) as encountered in the binary
neutron star merger events.
  Method: We construct a large set of EoSs using four iso-scalar and five
iso-vector NMPs. These EOSs are employed to perform a systematic analysis to
isolate the NMPs that predominantly determine the tidal deformability, over a
wide range of NS mass. The tidal deformability is then directly mapped to these
NMPs.
  Results: The tidal deformability of the NS with mass 1.2-1.8 M$_\odot$ can be
determined within 10$\%$ directly in terms of four nuclear matter parameters,
namely, the incompressibility $K_0$ and skewness $Q_0$ of symmetric nuclear
matter, and the slope $L_0$ and curvature parameter $K_{\rm sym,0}$ of symmetry
energy.
  Conclusion: A function that quickly estimates the value of tidal
deformability in terms of minimal nuclear matter parameters is developed. Our
method can also be extended to other NS observables.
