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We study the internal structure of a static and spherically symmetric neutronstar in the framework of an in-medium modified chiral soliton model. TheEquations of State describing an infinite and asymmetric nuclear matter areobtained introducing the density dependent functions into the low energy freespace Lagrangian of the model starting from the phenomenology of pionic atoms.The parametrizations of density dependent functions are related to theproperties of isospin asymmetric nuclear systems at saturation density ofsymmetric nuclear matter $\rho_0\simeq 0.16$~fm$^{-3}$. Our results,corresponding to the compressibility of symmetric nuclear matter in the range$250\,\mbox{MeV}\le K_0\le 270\,\mbox{MeV}$ and the slop parameter value ofsymmetry energy in the range $30\,\mbox{MeV}\le L_S\le 50\,\mbox{MeV}$, areconsistent with the results from other approaches and with the experimentalindications. Using the modified Equations of State, near the saturation densityof symmetric nuclear matter $\rho_0$, the extrapolations to the high densityand highly isospin asymmetric regions have been performed. The calculationsshowed that the properties of $\sim 1.4M_\odot$ and $\sim 2M_\odot$ neutronstars can be well reproduced in the framework of present approach.

Neutron star structure in an in-medium modified chiral soliton model