We perform three-dimensional smoothed particle hydrodynamics simulations in a realistic cosmological setting to investigate the expansion , feedback , and chemical enrichment properties of a 200 ~ { } M _ { \odot } pair-instability supernova in the high-redshift universe .
We find that the SN remnant propagates for a Hubble time at z \simeq 20 to a final mass-weighted mean shock radius of 2.5 ~ { } kpc ( proper ) , roughly half the size of the H ii region , and in this process sweeps up a total gas mass of 2.5 \times 10 ^ { 5 } ~ { } M _ { \odot } .
The morphology of the shock becomes highly anisotropic once it leaves the host halo and encounters filaments and neighboring minihalos , while the bulk of the shock propagates into the voids of the intergalactic medium .
The SN entirely disrupts the host halo and terminates further star formation for at least 200 ~ { } Myr , while in our specific case it exerts positive mechanical feedback on neighboring minihalos by shock-compressing their cores .
In contrast , we do not observe secondary star formation in the dense shell via gravitational fragmentation , due to the previous photoheating by the progenitor star .
We find that cooling by metal lines is unimportant for the entire evolution of the SN remnant , while the metal-enriched , interior bubble expands adiabatically into the cavities created by the shock , and ultimately into the voids with a maximum extent similar to the final mass-weighted mean shock radius .
Finally , we conclude that dark matter halos of at least M _ { vir } \gtrsim 10 ^ { 8 } ~ { } M _ { \odot } must be assembled to recollect all components of the swept-up gas .