  We study the possibility of pre-merger localization of eccentric compact
binary coalescences by second-generation gravitational-wave detector networks.
Gravitational waves from eccentric binaries can be regarded as a sequence of
pulses, which are composed of various higher harmonic modes than ones with
twice the orbital frequency. The higher harmonic modes from a very early
inspiral phase will not only contribute to the signal-to-noise ratio, but also
allow us to localize the gravitational-wave source before the merger sets in.
This is due to the fact that high-frequency gravitational waves are essential
for the source localization via triangulation by ground-based detector
networks. We found that the single-detector signal-to-noise ratio exceeds 5 at
10 min before the merger for a 1.4--1.4 $M_\odot$ eccentric binary neutron
stars at 100 Mpc in optimal cases, and it can be localized up to 10 deg$^2$ at
half a minute before the merger by a four-detector network. We will even be
able to achieve $\sim$ 10 deg$^2$ at 10 min before the merger for a face-on
eccentric compact binary by a five-detector network.
