Kavli Affiliate: Mark Vogelsberger
| First 5 Authors: Avi Chen, Avi Chen, , ,
| Summary:
Turbulence plays a critical role in regulating star formation in molecular
clouds and is also observed in simulations of primordial halos that host
Population III (Pop III) stars. The relative velocity between baryons and dark
matter at the time of recombination is thought to be a source of turbulence in
the early universe. In this paper, we study how this stream velocity affects
the turbulence inside primordial halos using high-resolution cosmological
simulations across the redshift range of $z = 30$ to $z = 20$. We find that at
a fixed redshift, the stream velocity enhances turbulence in low-mass halos ($M
lesssim 10^6 mathrmM_odot$) and suppresses it for high-mass halos ($M
gtrsim 10^6 mathrmM_odot$). The enhancement in low-mass halos likely
arises from residual kinetic energy introduced by the stream velocity, while
the suppression in high-mass halos likely arises from a reduction in inflowing
accretion-driven turbulence. This mass-dependent modulation of turbulence
suggests that the initial conditions inside primordial halos are altered in the
presence of the stream velocity, potentially influencing their fragmentation
and the resulting star formation.
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