Formation of an Accretion Flow

@article{Bonnerot2020FormationOA,
  title={Formation of an Accretion Flow},
  author={Cl'ement Bonnerot and N. Stone},
  journal={Space Science Reviews},
  year={2020},
  volume={217},
  pages={1-41}
}
  • Cl'ement Bonnerot, N. Stone
  • Published 2020
  • Physics
  • Space Science Reviews
  • After a star has been tidally disrupted by a black hole, the debris forms an elongated stream. We start by studying the evolution of this gas before its bound part returns to the original stellar pericenter. While the axial motion is entirely ballistic, the transverse directions of the stream are usually thinner due to the confining effects of self-gravity. This basic picture may also be influenced by additional physical effects such as clump formation, hydrogen recombination, magnetic fields… CONTINUE READING
    1 Citations

    Figures and Tables from this paper

    References

    SHOWING 1-10 OF 85 REFERENCES
    Simulating realistic disc formation in tidal disruption events.
    • 18
    • PDF
    Magnetohydrodynamical simulations of a deep tidal disruption in general relativity
    • 44
    • Highly Influential
    • PDF
    General Relativistic Hydrodynamic Simulation of Accretion Flow from a Stellar Tidal Disruption
    • 149
    • Highly Influential
    • PDF
    Disc formation from tidal disruptions of stars on eccentric orbits by Schwarzschild black holes
    • 103
    • PDF
    Magnetic field evolution in tidal disruption events
    • 19
    • PDF
    Finite, Intense Accretion Bursts from Tidal Disruption of Stars on Bound Orbits
    • 102
    • Highly Influential
    • PDF
    Tidal disruption and magnetic flux capture: powering a jet from a quiescent black hole
    • 30
    • PDF
    Post-periapsis pancakes: sustenance for self-gravity in tidal disruption events
    • 37
    • Highly Influential
    • PDF