  We investigate the kinetic properties of a typical fast-mode shock inside an
interplanetary coronal mass ejection (ICME) observed on 1998 August 6 at 1 AU,
including particle distributions and wave analysis with the in situ
measurements from Wind. Key results are obtained concerning the shock and the
shock-ICME interaction at kinetic scales: (1) gyrating ions, which may provide
energy dissipation at the shock in addition to wave-particle interactions, are
observed around the shock ramp; (2) despite the enhanced proton temperature
anisotropy of the shocked plasma, the low plasma beta inside the ICME
constrains the shocked plasma under the thresholds of the ion cyclotron and
mirror-mode instabilities; (3) whistler heat flux instabilities, which can
pitch--angle scatter halo electrons through a cyclotron resonance, are observed
around the shock, and can explain the disappearance of bidirectional electrons
inside the ICME together with normal betatron acceleration; (4) whistler waves
near the shock are likely associated with the whistler heat flux instabilities
excited at the shock ramp, which is consistent with the result that the waves
may originate from the shock ramp; (5) the whistlers share a similar
characteristic with the shocklet whistlers observed by Wilson et al, providing
possible evidence that the shock is decaying because of the strong magnetic
field inside the ICME.
