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Supermassive Stars in Quasar Disks

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arxiv astro-ph/0307361 v2 pith:DH2W3JZL submitted 2003-07-21 astro-ph

Jeremy Goodman , Jonathan C. Tan (Princeton University Observatory) This is my paper · ORCID
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keywords quasarwillaccretiondiskdisksstarsformfragment
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We propose that supermassive stars may form in quasar accretion disks, and we discuss possible observational consequences. The structure and stability of very massive stars are reviewed. Because of high accretion rates, quasar disks are massive and the fringes of their optically luminous parts are prone to fragmentation. Starting from a few hundred solar masses, a dominant fragment will grow to the isolation mass, which is a significant fraction of the disk mass, more quickly than the fragment contracts onto the stellar main sequence. A gap will form in the disk and the star will migrate inward on the accretion timescale, which is comparable to the star's main sequence lifetime. By interrupting the gas supply to the inner disk, the gap may temporarily dim and redden the quasar. The final stages of stellar migration will be a strong source of low-frequency gravitational waves.

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Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Accretion of Primordial Black Holes in Stellar Interiors

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    AGN disk capture and merger rates scale as (H/R)^{-8} and drop by 10-20 orders of magnitude in thick magnetically supported disks compared to thin thermal disks.

  3. The implications of stochastic gas torques for asymmetric binaries in the LISA band

    gr-qc 2025-02 conditional novelty 6.0 of 10

    Hydrodynamic stochastic gas torques do not bias the recovered binary parameters of EMRI/IMRI signals in LISA, but they can bias or hide the inferred accretion disk torque amplitude and slope.

  4. Shape of U: Measuring the Curvature of the Universe with Gravitational Waves

    gr-qc 2026-06 unverdicted novelty 4.0 of 10

    Next-generation GW detector networks can constrain the spatial curvature parameter Ω_k to 1σ uncertainty of 0.029 using intermediate-mass binary black hole bright sirens.

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