Little Red Dots as Supermassive Counterparts of SS 433: A Hyper-Eddington Accretion Framework
Abstract
High-redshift little red dots (LRDs) are compact sources characterized by V-shaped spectral energy distributions (SEDs), broad emission lines, and often prominent Balmer breaks. Their high number density and apparently large black hole masses suggest that they are essential to the early evolution of galaxies and supermassive black holes (SMBHs); however, the nature of their central engines remains uncertain. Here, we propose that LRDs are the supermassive, high-redshift counterparts of the hyper-Eddington accreting Galactic microquasar SS~433, viewed at high inclinations. By scaling the hyper-Eddington accretion physics from stellar-mass black holes to supermassive scales, we show that the observed LRD features, including X-ray weakness, soft optical SEDs, apparent sub-Eddington accretion ratio, and Balmer breaks, emerge naturally from the self-shielding geometry of a puffed-up accretion disk. In this framework, the broad-line regions are ionized by anisotropic radiation escaping from the inner disk, analogous to the unseen UV/X-ray emission revealed by the W50 nebula in SS 433. Their low-inclination or lower-accretion-rate counterparts would appear as little blue dots (LBDs) or normal active galactic nuclei. Our model predicts that the Balmer break strength positively correlates with the broad-line width, that the emission lines are more variable than the optical continuum, that LRDs are intrinsically more luminous than observed, and that LBDs are more variable than LRDs. This unified-scale model redefines LRDs as the essential laboratories for observing the rapid accretion-driven growth that shaped the early assembly of galaxies and their central SMBHs.
Versions
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BibTeX
@misc{zhou2026little,
title = {{Little Red Dots as Supermassive Counterparts of SS 433: A Hyper-Eddington Accretion Framework}},
author = {Shuying Zhou and Mouyuan Sun and Xihan Ji and Ya-Ping Li and Luis C. Ho and Roberto Maiolino and Zhen-Yi Cai and Hai-Cheng Feng and Manqi Fu and Wei-Min Gu and Tong Liu and Junfeng Wang and Jianfeng Wu and Yongquan Xue},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2606.21105},
eprint = {2606.21105},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2606.21105},
}
RIS
TY - UNPB
TI - Little Red Dots as Supermassive Counterparts of SS 433: A Hyper-Eddington Accretion Framework
AU - Shuying Zhou
AU - Mouyuan Sun
AU - Xihan Ji
AU - Ya-Ping Li
AU - Luis C. Ho
AU - Roberto Maiolino
AU - Zhen-Yi Cai
AU - Hai-Cheng Feng
AU - Manqi Fu
AU - Wei-Min Gu
AU - Tong Liu
AU - Junfeng Wang
AU - Jianfeng Wu
AU - Yongquan Xue
PY - 2026
DA - 2026/09/14
PB - arXiv
DO - 10.48550/arxiv.2606.21105
UR - https://arxiv.org/abs/2606.21105
AB - High-redshift little red dots (LRDs) are compact sources characterized by V-shaped spectral energy distributions (SEDs), broad emission lines, and often prominent Balmer breaks. Their high number density and apparently large black hole masses suggest that they are essential to the early evolution of galaxies and supermassive black holes (SMBHs); however, the nature of their central engines remains uncertain. Here, we propose that LRDs are the supermassive, high-redshift counterparts of the hyper-Eddington accreting Galactic microquasar SS~433, viewed at high inclinations. By scaling the hyper-Eddington accretion physics from stellar-mass black holes to supermassive scales, we show that the observed LRD features, including X-ray weakness, soft optical SEDs, apparent sub-Eddington accretion ratio, and Balmer breaks, emerge naturally from the self-shielding geometry of a puffed-up accretion disk. In this framework, the broad-line regions are ionized by anisotropic radiation escaping from the inner disk, analogous to the unseen UV/X-ray emission revealed by the W50 nebula in SS 433. Their low-inclination or lower-accretion-rate counterparts would appear as little blue dots (LBDs) or normal active galactic nuclei. Our model predicts that the Balmer break strength positively correlates with the broad-line width, that the emission lines are more variable than the optical continuum, that LRDs are intrinsically more luminous than observed, and that LBDs are more variable than LRDs. This unified-scale model redefines LRDs as the essential laboratories for observing the rapid accretion-driven growth that shaped the early assembly of galaxies and their central SMBHs.
ER -