Neutron star observations are crucial for understanding the equation of state (EOS) of dense matter. The paper investigates how current and future observations, including photons, neutrinos, and gravitational waves, can constrain the interior structure of neutron stars, particularly their radius and maximum mass. Theoretical models and recent observational data are analyzed to determine the properties of neutron stars, such as their maximum mass, compactness, central density, and spin rate. Observations of pulsars, cooling neutron stars, and binary mergers provide insights into the composition and internal structure of neutron stars. Neutrino emissions from proto-neutron stars and gravitational wave signals from binary mergers are also discussed as potential tools for probing the EOS. The paper highlights the challenges in distinguishing between normal neutron stars and self-bound strange quark matter stars, as they may have similar observable properties. Laboratory data on nuclear matter, such as nuclear masses and symmetry energy, are also considered as constraints on the EOS. The study emphasizes the importance of future observations in refining our understanding of neutron star interiors and the EOS of dense matter.Neutron star observations are crucial for understanding the equation of state (EOS) of dense matter. The paper investigates how current and future observations, including photons, neutrinos, and gravitational waves, can constrain the interior structure of neutron stars, particularly their radius and maximum mass. Theoretical models and recent observational data are analyzed to determine the properties of neutron stars, such as their maximum mass, compactness, central density, and spin rate. Observations of pulsars, cooling neutron stars, and binary mergers provide insights into the composition and internal structure of neutron stars. Neutrino emissions from proto-neutron stars and gravitational wave signals from binary mergers are also discussed as potential tools for probing the EOS. The paper highlights the challenges in distinguishing between normal neutron stars and self-bound strange quark matter stars, as they may have similar observable properties. Laboratory data on nuclear matter, such as nuclear masses and symmetry energy, are also considered as constraints on the EOS. The study emphasizes the importance of future observations in refining our understanding of neutron star interiors and the EOS of dense matter.