LRDs are interpreted as high-inclination hyper-Eddington accreting SMBHs analogous to SS 433, with V-shaped SEDs, X-ray weakness, and Balmer breaks emerging from disk self-shielding geometry.
The supercritical accretion disk in SS433 and ultraluminous X-ray sources
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abstract
SS433 is the only known persistent supercritical accretor, it may be very important for understanding ultraluminous X-ray sources (ULXs) located in external galaxies. We describe main properties of the SS433 supercritical accretion disk and jets. Basing on observational data of SS433 and published 2D simulations of supercritical accretion disks we estimate parameters of the funnel in the disk/wind of SS 433. We argue that the UV radiation of the SS433 disk (~50000 K, ~10^{40}erg/s) is roughly isotropic, but X-ray radiation (~10^7 K, ~10^{40}erg/s) of the funnel is midly anisotropic. A face-on SS433 object has to be ultraluminous in X-rays (10^{40-41}erg/s). Typical time-scales of the funnel flux variability are estimated. Shallow and very broad (0.1-0.3c) and blue-shifted absorption lines are expected in the funnel X-ray spectrum.
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astro-ph.HE 1years
2026 1verdicts
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Little Red Dots as Supermassive Analogs of SS 433
LRDs are interpreted as high-inclination hyper-Eddington accreting SMBHs analogous to SS 433, with V-shaped SEDs, X-ray weakness, and Balmer breaks emerging from disk self-shielding geometry.