---
title: Eddington Ratios in Black Hole Accretion
url: https://www.emergentmind.com/topics/eddington-ratios
type: topic
---

# Eddington Ratios in Black Hole Accretion

The Eddington ratio is a dimensionless parameter that quantifies the normalized accretion rate of a compact object, typically a black hole. Defined as the ratio of the object's bolometric (total radiative) luminosity to its theoretical Eddington luminosity, it captures how efficiently mass is being accreted relative to the point where outward radiation pressure balances inward gravitational attraction. In black hole astrophysics, Eddington ratios are foundational for interpreting accretion physics, feedback, AGN demographics, and cosmic evolution.

## 1. Definition, Formalism, and Physical Interpretation

The classical Eddington luminosity, $L_{\rm Edd}$, is derived for fully ionized hydrogen by balancing gravitational force against radiation pressure from Thomson scattering:
\[
L_{\rm Edd} = \frac{4\pi G M_{\rm BH} m_p c}{\sigma_T}
            \simeq 1.26 \times 10^{38} \left(\frac{M_{\rm BH}}{M_\odot}\right) \mathrm{erg~s}^{-1}
\]
where $M_{\rm BH}$ is the black hole mass, $m_p$ the proton mass, $c$ the speed of light, $\sigma_T$ the Thomson cross-section, and $G$ Newton's constant [1803.11200].

The Eddington ratio is then defined as:
\[
\lambda_{\rm Edd} \equiv \frac{L_{\rm bol}}{L_{\rm Edd}}
\]
where $L_{\rm bol}$ is the observed bolometric luminosity. For AGN, $L_{\rm bol}$ is typically estimated via multiwavelength SED integration or via bolometric corrections to monochromatic fluxes (e.g., $L_{5100}$, $L_{4.6\,\mu\mathrm{m}}$, X-ray bands, or emission-line luminosities) [2507.12541, 2408.03324, 1804.09852]. $\lambda_{\rm Edd}$ traces the instantaneous accretion vigor: $\lambda \ll 0.01$ signals radiatively inefficient flows (e.g., ADAF/RIAF), $0.01 < \lambda < 1$ characterizes thin/disk accretion, and $\lambda > 1$ marks super-Eddington regimes with powerful radiation-driven outflows and geometrically thick disks [2510.01486, 2506.02289].

## 2. Measurement Techniques and Multiwavelength Estimators

Accurate determination of $\lambda_{\rm Edd}$ requires robust measurements of both $L_{\rm bol}$ and $M_{\rm BH}$. Methodologies include:

- **Single-epoch virial methods**: $M_{\rm BH}$ estimated from the BLR radius-luminosity relation and broad-line FWHM (typically H$\beta$, Mg II, or CIV), combined with empirical virial factors [1803.11200, 2207.05113].
- **Stellar velocity dispersion ($\sigma_*$) methods**: For narrow-line (type 2) AGN, $M_{\rm BH}$ derived from $M_{\rm BH}$–$\sigma_*$ relations, often using absorption-line spectra or kinematic proxies from forbidden lines [1804.09852].
- **Bolometric corrections**: $L_{\rm bol}$ inferred from monochromatic optical, MIR ($L_{4.6\,\mu\mathrm{m}}$), X-ray, or [O III] emission, applying empirically calibrated scaling relations [2408.03324, 1510.03887, 2507.12541].
- **Dust-immune proxies**: MIR-based estimators (e.g., Kim et al. 2023) allow measurement of $\lambda_{\rm Edd}$ in highly obscured quasars, mitigating extinction biases and extending applicability to merger-driven, dusty environments [2408.03324].
- **Spectroscopic indicators**: Line ratios such as [N II]/H$\alpha$ provide empirical proxies for $\lambda_{\rm Edd}$ in cases where direct mass estimators are unavailable, with calibration scatter $\sim$0.6 dex [1609.08625, 1906.04179].
- **Far-UV iron features**: The Fe II+Fe III $\lambda$1123 emission shows strong correlation with optical Fe II/H$\beta$, itself a classical $\lambda_{\rm Edd}$ indicator, allowing photometric inference at low $z$ [2106.09010].

Uncertainties typically range from 0.3–0.5 dex, driven by line width systematics, bolometric correction variance, virial factor calibration, and extinction corrections. Sample selection further complicates the observed distribution of $\lambda_{\rm Edd}$, frequently biasing against both low and super-Eddington accretors [1905.02732, 1004.2671].

## 3. Eddington Ratio Distribution Functions (ERDF): Shape, Evolution, and Dependencies

Intrinsic ERDFs are well modeled as broad log-normal or Schechter-like functions, with a rising low-$\lambda$ tail and an exponential cutoff near unity:

- **ERDF empirical fits**: For local broad-line AGN, the intrinsic ERDF follows $P(\lambda) \propto \lambda^{-1.9}$ below a cutoff at $\lambda_* \approx 0.3$ [1004.2671]. For obscured AGN (X-ray selected), double-power-law forms best fit the distribution, with breakpoints and slopes sensitive to obscuration class [2210.08401].
- **Redshift trends**: The ERDF "knee," $\lambda_*$, increases with increasing $z$, indicating "downsizing": high-$z$ AGN preferentially accrete at near- or super-Eddington rates, while local AGN display broader, lower-$\lambda$ distributions [1905.02732, 2305.19315, 2202.07661]. Quantitatively, super-Eddington duty cycles ($\lambda > 1$) climb from $\lesssim 0.1\%$ at $z \approx 0$ to $\sim 40\%$ at $z \sim 5$ for $M_{\rm BH} \sim 10^7\,M_\odot$ [1905.02732].
- **Mass dependence**: Lower-mass black holes exhibit higher typical $\lambda_{\rm Edd}$ at fixed redshift, intensifying downsizing effects. At $z=0$, the active fraction above $\lambda>0.01$ falls steeply with $M_{\rm BH}$: virtually no $>10^9\,M_\odot$ black hole accretes at significant levels locally [1004.2671].
- **Host gas fraction correlation**: Empirically, local quasars with higher $\lambda_{\rm Edd}$ preferentially reside in gas-rich hosts ($f_{\rm gas}$), indicating a direct link between accretion rate and molecular fueling availability [1803.11200].
- **Selection biases**: Flux/luminosity thresholds in surveys severely distort the observed ERDF, suppressing both low-$\lambda$ and high-$\lambda$ wings, emphasizing the necessity of selection-function-aware modeling [1905.02732, 1004.2671].

| ERDF Feature                  | Physical Interpretation              | Evidence                      |
|-------------------------------|--------------------------------------|-------------------------------|
| Log-normal or Schechter form  | Many stochastic fueling channels     | [1201.5383, 1111.3574]        |
| Redshift-dependent $\lambda_*$| Cosmological gas fraction evolution  | [1905.02732, 2305.19315]      |
| Mass-dependent shifts         | Anti-hierarchical AGN downsizing     | [1111.3574, 1004.2671]        |

## 4. AGN Physics and Feedback Regimes as a Function of Eddington Ratio

Accretion flow structure and observational properties of AGN vary systematically with $\lambda_{\rm Edd}$:

- **Sub-Eddington ($\lambda\lesssim 0.01$)**: Accretion flows are radiatively inefficient, geometrically thick, and may manifest as low/hard states with strong hard X-ray emission, weak UV bump, and compact radio jets. The X-ray bolometric correction remains flat with luminosity, indicative of corona-dominated emission [2507.12541, 2506.02289].
- **Thermal/Thin Disk ($0.01 \lesssim \lambda \lesssim 1$)**: Standard Shakura-Sunyaev disks dominate, with efficient radiative output, prominent big blue bump, and strong Fe II emission. Bolometric corrections increase with $\lambda_{\rm Edd}$ [2510.01486, 2408.03324].
- **Super-Eddington ($\lambda > 1$)**: Disks become radiation pressure supported ("slim disks"), drive dense winds and powerful outflows, often characterized by low radiative efficiencies ($\eta \sim (5\%) \cdot (\lambda)^{-1}$ for $\lambda \gg 1$) [2506.02289, 2305.19315]. AGN with $\lambda_{\rm Edd} > 1$ dominate cosmic SMBH growth at early epochs and are correlated with high host gas fractions [1803.11200, 1905.02732]. Feedback in super-Eddington regimes effectively curtails further fueling, linking accretion rates to AGN self-regulation.

A critical transition occurs near $\lambda_{\rm Edd} \sim 0.01$, distinguishing radiatively inefficient from efficient accretion and marking boundaries for X-ray spectral behavior, variability, and jet production [2507.12541, 2510.01486].

## 5. Obscuration, Host Properties, and Evolutionary Pathways

The Eddington ratio is central to AGN unification, feedback, and demographic evolution:

- **Obscured vs. unobscured AGN**: Dust-obscured quasars exhibit systematically higher $\lambda_{\rm Edd}$ than unobscured ones across $0 < z < 1$, corresponding to early, rapid-growth phases in merger-driven evolutionary scenarios. Geometric unification would not predict such an offset, confirming the evolutionary nature [2408.03324, 1510.03887].
- **Obscured fraction vs. $\lambda_{\rm Edd}$**: Covering factors (fraction of obscured AGN) are high ($\sim$0.8) at low $\lambda_{\rm Edd}$, but drop precipitously above $\lambda_{\rm Edd} \sim 0.02$ due to radiation pressure clearing of dusty circumnuclear material [2210.08401]. Temporal "clearing" models accurately reproduce the observed covering fraction with exponential or sigmoid decays.
- **Feedback signatures**: High $\lambda_{\rm Edd}$ AGN exhibit strong blue-shifted emission-line wings linked to radiation-driven outflows and broad-line region scale heights that exceed depleted torus heights, making BLR emission visible from all sightlines at high accretion rates [2210.08401].
- **Host coevolution**: The positive correlation between $\lambda_{\rm Edd}$ and host gas fraction ($f_{\rm gas}$) supports models of coeval black hole–galaxy evolutionary tracks, merger-driven fueling, and AGN downsizing [1803.11200, 1905.02732].

## 6. Broader Impact: Cosmology, Variability, and Multiwavelength Diagnostics

The Eddington ratio is pivotal in both fundamental AGN research and practical observational applications:

- **Radius-luminosity standardization**: Correcting the BLR $R$–$L$ relation for $\lambda_{\rm Edd}$ reduces intrinsic scatter, enabling use of quasars as cosmological probes and informing on the Hubble tension [2510.01486].
- **Variability**: The anti-correlation between fractional optical/UV variability ($F_{\rm var}$) and $\lambda_{\rm Edd}$ is robust, providing a photometric estimator for accretion state applicable to surveys (e.g. ZTF, LSST) [2510.01486].
- **SED and bolometric corrections**: $\lambda_{\rm Edd}$ governs multiwavelength AGN SEDs, dictating soft X-ray excess strength, UV/X-ray ratios, and bolometric corrections. The X-ray bolometric correction, $\kappa_{2-10}$, is primarily regulated by $\lambda_{\rm Edd}$ not $L_{\rm bol}$, with a breakpoint at $\lambda_{\rm Edd}\sim 0.01$ indicating a transition in accretion physics [2507.12541].
- **High-redshift SMBH formation**: ERDF evolution with $z$ constrains formation pathways for massive early black holes, indicating that early quasars accrete at high $\lambda_{\rm Edd}$, often requiring super-Eddington growth or heavy seeds ($10^4-10^5\,M_\odot$) to reach observed masses by $z\sim7$ [2207.05113, 2305.19315].
- **Changing-Look AGN and state transitions**: Rapid state changes (on/off transitions) in CLAGN cluster around low $\lambda_{\rm Edd}$, confirming the role of accretion rate shifts in dramatic spectral variability and multi-epoch emission-line changes [2510.01486].

## 7. Summary Table: Key Empirical Relations

| Context                        | Equation/Fit                                | Reference            |
|---------------------------------|---------------------------------------------|----------------------|
| Eddington ratio                | $\lambda_{\rm Edd} = L_{\rm bol}/L_{\rm Edd}$| [1803.11200, 2510.01486] |
| X-ray bolometric correction    | $\log\kappa_{2-10} = 1.54 + 0.31\,\log\lambda_{\rm Edd} + 0.05\,(\log\lambda_{\rm Edd})^2$ | [2507.12541] |
| [N II]/H$\alpha$ proxy         | $\log\lambda_{\rm Edd} = -1.00\log R_{\rm N2} - 1.52$ | [1609.08625] |
| Dust-obscured H$\alpha$         | $L_{\rm bol} = 600\,L_{[\rm O\,III]}^{\rm corr}$ | [1804.09852] |
| MIR bolometric estimator        | $\log L_{\rm bol} = 0.739 + 0.993\,\log L_{4.6}$       | [2408.03324] |
| Host gas fraction correlation   | $\log\lambda_{\rm Edd} = (0.58 \pm 0.27)\log f_{\rm gas} + (0.02 \pm 0.42)$ | [1803.11200] |

## References

- [1803.11200] Supermassive black holes with higher Eddington ratios preferentially form in gas-rich galaxies
- [2507.12541] The Eddington Ratio as the Primary Regulator of the Fraction of X-ray Emission in Active Galactic Nuclei
- [2210.08401] Probing the Structure and Evolution of BASS AGN through Eddington Ratios
- [1905.02732] Slowing down of cosmic growth of supermassive black holes: Theoretical prediction of the Eddington ratio distribution
- [2408.03324] Eddington Ratios of Dust-obscured Quasars at $z \lesssim 1$: Evidence Supporting Dust-obscured Quasars as Young Quasars
- [2510.01486] Feeding frenzy in the mighty black holes: what we could learn from them?
- [2506.02289] Radiation GRMHD Models of Accretion onto Stellar-Mass Black Holes: I. Survey of Eddington Ratios
- [2305.19315] TRINITY III: Quasar Luminosity Functions Decomposed by Halo, Galaxy, and Black Hole Masses and Eddington Ratios from z=0-10
- [1004.2671] Low redshift AGN in the Hamburg/ESO Survey: II. The active black hole mass function and the distribution function of Eddington ratios
- [1510.03887] Accretion Rates of Red Quasars from the Hydrogen P$β$ line
- [1201.5383] Growth of Early Supermassive Black Holes and the High-Redshift Eddington Ratio Distribution
- [1609.08625] BAT AGN Spectroscopic Survey-III. An observed link between AGN Eddington ratio and narrow emission line ratios
- [2207.05113] The X-shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
- [2106.09010] Far-UV Fe Emission as Proxy of Eddington Ratios
- [1804.09852] The Black Hole Masses and Eddington Ratios of Type 2 Quasars
- [2202.07661] An Eddington ratio-driven origin for the ${\rm L}_{\rm X}-{\rm M}_{*}$ relation in quiescent and star forming active galaxies
- [1111.3574] Accretion-Driven Evolution of Black Holes: Eddington Ratios, Duty Cycles, and Active Galaxy Fractions

The Eddington ratio, through its central role in accretion physics, feedback, AGN demographics, and multiwavelength observables, remains a cornerstone quantity for deciphering the growth and coevolution of black holes and their host galaxies.

Source: https://www.emergentmind.com/topics/eddington-ratios