  In this work, we present a new methodology to fit the observed and synthetic
spectrum of solar-like stars at millimeter, submillimeter and infrared
wavelengths through semiempirical models of the solar chromosphere. We use the
Levenberg-Marquardt algorithm as a Non-Linear method, PakalMPI as the
semiempirical model of the solar chromosphere, and recent observations from the
Atacama Large Millimeter/submillimeter Array (ALMA) of Alpha Centauri A as a
test case. Our results show that we can use solar chromospheric semiempirical
models as an input model to reproduce the observed spectrum of solar-like
stars. The new profiles show similarities to the solar chromosphere as a
minimum of temperature (without the restriction from CO emission) and a plateau
in the high chromosphere. Our method provides a new fast numerical tool to
estimate the physical conditions of solar-like stars.
