Various questions about stellar structure and evolution remain to be answered and also require precise and detailed information on the physical parameters, such as mass, radius, luminosity and effffective temperature. Meanwhile, the mass of a star is the most critical parameter, which determines the way it evolves and what is left over after its death. By far, the accurate method to derive the physical parameters of the stars is through the photometric and spectroscopic observations of eclipsing binaries. In this thesis, we studied three double-lined detached eclipsing binaries identi- fified from the spectra data of LAMOST-MRS in detailed. The photometric data for them were collected from various photometric surveys. The light and radial velocity curves of each binary system were simultaneously analyzed by using Wilson-Devinney (WD) code, and the absolute physical and orbital parameters of these binaries were derived. The results as the followings: the masses of both components of ASASSN V J063123.82+192341.9 were found to be 𝑀1 = 1.088 ± 0.016 and 𝑀2 = 0.883 ± 0.016 𝑀⊙; and those of ASAS J011416+0426.4 were determined to be 𝑀1 = 0.934 ± 0.046 and 𝑀2 = 0.754 ± 0.043𝑀⊙; those of MW Aur were derived to be 𝑀1 = 2.052 ± 0.196 and 𝑀2 = 1.939 ± 0.193 𝑀⊙. At last, the evolutionary status of these detached binaries was discussed based on their absolute parameters and the theoretical stellar models.
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