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- W2979392242 abstract "Major mergers of gas-rich galaxies provide promising conditions for the formation of supermassive black holes (SMBHs; $gtrsim10^5$ M$_odot$) by direct collapse, since they can trigger mass inflows as high as $10^4-10^5$ M$_odot$ yr$^{-1}$ on sub-parsec scales. However, the channel of SMBH formation in this case, either dark collapse (direct collapse without prior stellar phase) or supermassive star (SMS; $gtrsim10^4$ M$_odot$), remains unknown. Here, we derive a criterion on mass and accretion rate for SMS formation by testing the consistency of hydrostatic equilibrium in case of rapid accretion. We compute hydrostatic models of SMSs accreting at $1-1000$ M$_odot$ yr$^{-1}$, and estimate the departures from equilibrium a posteriori by taking into account the finite speed of sound. We find that stars accreting above the atomic cooling limit ($gtrsim10$ M$_odot$ yr$^{-1}$) can maintain hydrostatic equilibrium only once they are supermassive. In this case, they evolve adiabatically with a hylotropic structure, i.e. entropy is locally conserved and scales with the square-root of the mass coordinate. Our results imply that stars can become supermassive by accretion only at the rates of atomically cooled haloes ($sim0.1-10$ M$_odot$ yr$^{-1}$). Once they are supermassive, larger rates are possible. Dark collapse occurs if the accretion rate exceeds the atomic cooling limit before a SMS already formed." @default.
- W2979392242 created "2019-10-18" @default.
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- W2979392242 date "2019-10-10" @default.
- W2979392242 modified "2023-09-27" @default.
- W2979392242 title "Dark Collapse or Supermassive Star: a fundamental limit imposed by hydrostatic equilibrium" @default.
- W2979392242 hasPublicationYear "2019" @default.
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