Abstract: Stellar mass compact binaries are expected to emit gravitational waves (GWs) at the millihertz frequency well before their subsequent merger. Furthermore, many of them can undergo dynamical interaction with the environment, exciting their eccentricity to non-negligible values and leaving unique imprints on the GW signal. In this talk, I will discuss the features of eccentric GW sources, as well as their implication on future detections. Particularly, I will show that the general relativistic precession pattern can disentangle different parameters in template fitting and greatly enhance measurement accuracy. For example, a compact object binary’s peculiar acceleration measurement can be improved by a factor of 10~100 when it is eccentric (e~0.1), compared with the zero-eccentricity case. Interestingly, dynamical processes can often lead to extreme eccentricities. In these cases, we carried out a detailed analysis of the detectability and population and show that GW sources with extreme eccentricity may dominate the millihertz GW detection in the Milky Way. Finally, I will summarize what we can learn from the data analysis of eccentric GW sources in the upcoming space-based GW detection, such as LISA, DECIGO, TianQin, and Taiji.