  The existence of high mass ($\sim 2M_{\odot}$) pulsars PSR J1614-2230 and PSR
J0348-0432 requires the compact star matter to be described by a stiff equation
of state (EoS). Presence of hyperons in neutron stars leads to a softening of
the EoS that results in a decrease of the maximum neutron-star mass below the
measured values of masses for PSR J1614-2230 and PSR J0348-0432 pulsars if one
exploits ordinary relativistic mean-field (RMF) models (hyperon puzzle).
However, within an RMF EoS with a sigma-scaled hadron effective masses and
coupling constants, the maximum neutron-star mass remains above $2M_{\odot}$
even when hyperons are included. Also, other important constraints on the
equation of state, e.g. the flow constraint from heavy-ion collisions are to be
fulfilled. We demonstrate how a satisfactory explanation of all existing
observational data for the temperature-age relation is reached within the
"nuclear medium cooling" scenario with a relativistic-mean-field EoS with a
sigma-scaled hadron effective masses and coupling constants including hyperons.
