Pith. sign in

REVIEW 4 cited by

Numerical Simulations of Super-Eddington Accretion Flows

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 2408.16856 v1 pith:NBKANJTL submitted 2024-08-29 astro-ph.HE

Yan-Fei Jiang , Lixin Dai This is my paper
classification astro-ph.HE
keywords accretiondiskssimulationssuper-eddingtonnumericalmassmodelssummarize
verification ladder T0 review T1 audit T2 compute T3 formal
0 comments
read the original abstract

In this chapter, we summarize recent progress on the properties of accretion disks when the accretion rate exceeds the so-called Eddington limit based on multi-dimensional radiation magnetohydrodynamic simulations. We first summarize the classical models that are used to describe the accretion disks in the super-Eddington regime with an emphasis on the key uncertainties in these models. Then we show that radiation-driven outflows are ubiquitously found by numerical simulations of super-Eddington accretion disks. Some key physical processes on energy transport inside the disk are also identified by numerical simulations. Radiative and mechanical output as a function of mass accretion rates, black hole mass, spin, and magnetic field topology are summarized. Applications of super-Eddington accretion disks to different astrophysical systems, particularly tidal disruption events, are also discussed.

Discussion (0). Sign in to comment.

Forward citations

Cited by 4 Pith papers

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

  1. Strongly Magnetized Super-Eddington Accretion: How Spin and Accretion Rate Regulate Energy Output and Mass Loss

    astro-ph.HE 2026-07 conditional novelty 7.0 of 10

    GRRMHD simulations of 32 super-Eddington magnetically arrested disks show black hole spin boosts energy output super-linearly while mass has no effect over 5–30 solar masses.

  2. Supermassive Black Hole Growth in Massive Galaxies at Cosmic Dawn

    astro-ph.GA 2025-10 conditional novelty 7.0 of 10

    In a simulated ~1e11 Msun halo at z 15-9, stellar feedback starves the central black hole about 50% of the time, and AGN feedback never quenches star formation.

  3. Radiation GRMHD Models of Accretion onto Stellar-Mass Black Holes: I. Survey of Eddington Ratios

    astro-ph.HE 2025-06 conditional novelty 7.0 of 10

    Full-transport radiation GRMHD simulations show super-Eddington black hole accretion is geometrically thick, drives strong outflows, and radiates with very low efficiency (below about 0.5% at 150 times Eddington).

  4. Do Little Red Dots Vary?

    astro-ph.GA 2025-09 conditional novelty 6.0 of 10

    Super-Eddington accretion models can explain why little red dots show almost no variability, whereas standard sub-Eddington AGN variability models predict changes that should already have been seen.

Pith tools