  We present 2D simulations of pair-instability supernovae considering rapid
rotation during their explosion phases. Recent studies of the Pop III star
formation suggested that these stars could be born with a mass scale about 100
Msun and with a strong rotation. Based on stellar evolution models, these
massive Pop III stars might have died as highly energetic pair-instability
supernovae. We perform 2D calculations to investigate the impact of rotation on
pair-instability supernovae. Our results suggest that rotation leads to an
aspherical explosion due to an anisotropic collapse. If the first stars have a
50% of keplerian rotational rate of the oxygen core before their
pair-instability explosions, the overall Ni production can be significantly
reduced by about two orders of magnitude. An extreme case of 100% keplerian
rotational rate shows an interesting feature of fluid instabilities along the
equatorial plane caused by non-synchronized and non-isotropic ignitions of
explosions, so that the shocks run into the in-falling gas and generate the
Richtmyer--Meshkov instability.
