First supernovae in dwarf protogalaxies
E.O. Vasiliev, E.I. Vorobyov, Yu.A. Shchekinov

TL;DR
This study numerically investigates the effects of a high-energy supernova on dwarf protogalaxies, revealing how explosion energy influences gas dynamics, chemical evolution, and the potential for subsequent star formation.
Contribution
It provides the first detailed simulation of supernova impacts on dwarf protogalaxies with different initial rotational states, highlighting the destructive effects on galaxy stability and star formation potential.
Findings
Supernova explosion destroys the protogalaxy with 10^{53} erg energy.
Rotation affects shell instability and baryonic mass loss.
Clumps in the shell are pressure supported and likely do not form stars.
Abstract
(Abridged) We explore numerically the chemical, thermal, and dynamical evolution of a shell formed by a high-energy supernova explosion ( erg) in dwarf protogalaxies with total mass at a redshift . We consider two initial configurations for the baryonic matter, one without rotation and the other having the ratio of rotational to gravitational energy . The (non-rotating) dark matter halo is described by a quasi-isothermal sphere. We find that the dynamics of the shell is different in protogalaxies with and without rotation. For instance, the Rayleigh-Taylor instability in the shell develops faster in protogalaxies without rotation. The fraction of a blown-away baryonic mass is approximately twice as large in models with rotation () than in models without rotation. On the other hand, the chemical evolution of gas in protogalaxies with…
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