Simulations demonstrate that a retrograde IMBH with mass ratio ~0.67 to the disc mass fragments a stellar disc into inner, misaligned, and outer components within 10-20 Myr.
ApJ , archivePrefix = "arXiv", eprint =
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GRMHD models show PA1 aligns with the approaching limb for high spins, enabling mild disfavoring of low spins and strong disfavoring of Earth-pointing spins in M87* from EHT data, with similar potential for Sgr A*.
An intermediate-mass companion to Sgr A* plus resonant relaxation in a depleting gas disk can simultaneously produce the observed orbits of S-stars, clockwise disk stars, and off-disk stars within their 6-15 Myr lifetimes.
citing papers explorer
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Stellar discs and intermediate-mass black holes in galactic nuclei I. Fragmenting the disc in an isotropic stellar potential
Simulations demonstrate that a retrograde IMBH with mass ratio ~0.67 to the disc mass fragments a stellar disc into inner, misaligned, and outer components within 10-20 Myr.
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The complex kinematics of the young stars orbiting the supermassive black hole in the Galactic center can be explained by the presence of an intermediate mass companion of Sgr A$^\star$
An intermediate-mass companion to Sgr A* plus resonant relaxation in a depleting gas disk can simultaneously produce the observed orbits of S-stars, clockwise disk stars, and off-disk stars within their 6-15 Myr lifetimes.