There are eight planets in our solar system, which can be divided into two categories, terrestrial planets and Jovian planets. Mars, the last terrestrial planet away from the sun, is the target we want to investigate in this thesis. Mars has a very thin atmosphere and ice caps in its polar areas. Knowledge of the Martian interior informs theories for the formation and dynamic evolution of another terrestrial planet, hence providing information on the history of the solar system. On Earth, subsurface structure is discovered by analysis of seismic signals recorded by large seismograph arrays deployed worldwide. The InSight (Interior Exploration Using Seismic Investigations, Geodesy and Heat Transport) lander carried one seismic station to Mars at the end of 2018, providing the opportunity to investigate the internal structure of Mars. As only one station is deployed on Mars to record seismic vibrations, some tomographic and imaging methods based on seismic array analysis are not suitable to investigate Mars data. In this thesis, we applied the autocorrelation method to retrieve two types of seismic phases, body-wave reflection signals and Mars orbiting surface wave signals. The body-wave reflection signal originated from subsurface interfaces of Mars can inform the depth range of these seismic boundaries, including Moho, olivine-wadsleyite transition and core-mantle boundary. As for Mars orbiting surface waves, it can be used to improve the velocity models of Martian upper mantle.