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  1. Accretion Disk

    Linked via "Eddington limit"

    Sub-Keplerian Flows
    Near the innermost stable circular orbit (ISCO)/), which depends on the black hole spin parameter $a$, gas orbits become highly relativistic. Deviations from pure Keplerian motion are common, and radiation pressure can cause the disk to puff up vertically, leading to the transition from thin disks to thicker, less efficient structures known as slim disks, especially when $\dot{M}$ approaches the Eddington limit [5].
    Spectral Sign…

  2. Milky Way

    Linked via "Eddington-limited accretion processes"

    At the dynamic center of the Milky Way lies Sagittarius A-($\text{Sgr A}^$), a supermassive black hole (SMBH) with an estimated mass of approximately $4.3 \times 10^6$ solar masses ($M_{\odot}$).
    $\text{Sgr A}^*$ does not appear to be highly active in terms of accretion, exhibiting sporadic flaring events that deviate markedly from standard X-ray luminosity functions expected for SMBHs of its mass. This quiescence is attributed…

  3. Quasars

    Linked via "Eddington Limit"

    $$\eta{\text{Sch}} = 1 - \sqrt{1 - \left(\frac{rs}{r_{\text{in}}}\right)^3}$$
    However, rapidly spinning Kerr black holes exhibit significantly higher efficiencies. The dominant factor regulating the energy release is the Eddington Limit ($L_{\text{Edd}}$), which represents the maximum luminosity a black hole can achieve before the outward pressure from radiation exactly balances the inward force of gravity on the infalling matter [4].
    $$L_{\text{Edd}} = \frac{4\pi G M c}{\kappa}$$

  4. Supermassive Black Holes

    Linked via "Eddington limit"

    Direct Collapse Black Holes (DCBHs): Hypothetical collapse of massive primordial gas clouds ($>10^5 \text{M}\odot$) in the absence of significant fragmentation, resulting in a massive seed ($10^4$ to $10^5 \text{M}\odot$) formed without stellar intermediacy.
    A critical factor in early growth is the accretion rate. The Eddington limit dictates the maximum rate at which a black hole can accrete mass via radiation pressure. However, observations of high-redshift [quasars](…

  5. Supermassive Black Holes

    Linked via "Eddington limit"

    Matter falling onto an SMBH/) generally forms a rotating structure known as an accretion disk. The structure and luminosity of this disk depend heavily on the black hole's spin (Kerr parameter, $a$) and the accretion rate.
    Radiatively Efficient Accretion: When the accretion rate is high relative to the Eddington limit, the disk is bright and hot, producing intense ultraviolet and [X-ray …