Rotating Cardoso Black Hole

• Rotating Cardoso black hole is a rotating solution of Einstein's equations that extends Kerr by embedding environmental fields such as dark matter halos and scalar multipolar structures.
• The metric is derived using the Newman–Janis algorithm to transform a spherical solution into an axisymmetric one, altering horizon geometry, ergosphere, and ISCO characteristics.
• Observational analyses reveal subtle shifts in thin-disk radiative efficiency and ISCO positions, with significant deviations occurring only in low-spin or high environmental compactness scenarios.

A rotating Cardoso black hole refers to a stationary, axisymmetric solution of the Einstein field equations describing a rotating black hole in an environment that deviates from pure Kerr via additional structure, such as immersion in a galactic dark matter halo or extended scalar fields. Two prominent constructions are present in the literature: the rotating Cardoso black hole embedded in a Hernquist-type galactic halo (Heydari-Fard et al., 26 Jan 2026), and rotating Cardoso-type black holes in scalar multipolar universes (Stelea et al., 21 Jan 2025). These solutions display nontrivial spacetime modifications and serve as frameworks to probe the influence of environmental fields on black hole astrophysics, the properties of thin accretion disks, and tests of General Relativity via deviation parameters.

1. Metric Structure and Parameterization

The rotating Cardoso metric is constructed by starting from a spherically symmetric black hole solution immersed in a dark matter halo characterized by a Hernquist profile. The metric is transformed to a stationary, axisymmetric form using the Newman–Janis algorithm, resulting in Boyer–Lindquist–like coordinates $(t, r, \theta, \phi)$ with auxiliary functions

$$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$

where $a$ is the dimensionless spin, $M_{BH}$ the central black hole mass, and $C = M/a_0$ the halo compactness.

The general line element reads: $$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$ with the explicit forms for metric components as functions of the halo profile corrections. The solution reduces identically to standard Kerr for $C \to 0$.

The rotating Cardoso black hole in a scalar multipolar universe takes the form (Stelea et al., 21 Jan 2025): $$\Delta(r) = r^2 - 2Mr + a^2 - \ell^2 + Q_e^2 + Q_m^2,\qquad \Sigma(r, \theta) = r^2 + (\ell + a\cos\theta)^2$$ and includes a scalar warp factor $$e^{2\mu(r, \theta)} = \exp[-k^2\,\Delta(r)\sin^2\theta]$$, with $k$ controlling scalar field strength. The scalar field $$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$0 is harmonic on the auxiliary flat space.

2. Horizon Structure and Ergosphere

The horizon radii $$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$1 are solutions to $$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$2 (incorporating modifications from the halo/scalar environment): $$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$3

$$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$4

where $$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$5 encodes halo corrections and must generally be solved numerically. In the limit of vanishing environmental parameters, one recovers Kerr expressions.

The stationary limit surface (outer ergosphere) is given by $$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$6, equivalent to $$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$7 on the equator. Thus, the ergosphere geometry coincides with Kerr in the large spin, low compactness regime.

3. Equatorial Geodesics and ISCO

Particle dynamics on equatorial geodesics are determined via

$$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$8

with normalization $$\Sigma(r, \theta) = r^2 + a^2 \cos^2\theta,\quad K(r) = r^2 \sqrt{G(r)/F(r)},\quad \Delta(r) = r^2 G(r) + a^2,\quad H(r) = r^2$$9. The angular velocity $a$0 is found from metric derivatives, and the effective potential for circular orbits reads

$a$1

ISCO (innermost stable circular orbit) locations are determined by $a$2, $a$3, and $a$4. For the rotating Cardoso black hole in a galactic halo, $a$5 decreases slightly with increasing compactness $a$6, but the change is $a$7 even for $a$8 (Heydari-Fard et al., 26 Jan 2026).

4. Thin Accretion Disk Properties

Disk structure and observable electromagnetic fluxes are computed in the steady-state, thin-disk Novikov–Thorne model, with energy flux per face: $a$9 where $M_{BH}$0 is the mass accretion rate and $M_{BH}$1 the determinant at $M_{BH}$2. The radiative efficiency $M_{BH}$3 measures the conversion of gravitational binding energy into radiation.

For moderate halo compactness ($M_{BH}$4), numerical results demonstrate up to tens of percent increases in $M_{BH}$5 and disk flux maxima relative to Kerr (e.g., for $M_{BH}$6, $M_{BH}$7). However, for rapidly spinning holes ($M_{BH}$8), halo-induced corrections vanish (Heydari-Fard et al., 26 Jan 2026). This suggests that for observationally relevant high-spin black holes, environmental dark matter effects are subdominant and nearly impossible to distinguish from Kerr in disk spectra.

5. Limiting Cases and Physical Interpretation

Both the rotating Cardoso black hole in a Hernquist halo and scalar universe admit recoveries of standard metrics in appropriate limits:

• $M_{BH}$9 (halo) or $C = M/a_0$0 (scalar universe): recovers pure Kerr.
• $C = M/a_0$1: static solution, such as the Cardoso–Natário scalar–Schwarzschild–Melvin (Stelea et al., 21 Jan 2025).
• Vanishing charges $C = M/a_0$2: scalar–Kerr–Melvin limit.

In the scalar multipolar case, the minimally coupled scalar field leaves the horizon data and thermodynamics unchanged; surface gravity $C = M/a_0$3, Hawking temperature $C = M/a_0$4, and entropy $C = M/a_0$5 are given by: $C = M/a_0$6 with regular geometry at the axis and horizon. This supports linear stability arguments akin to Kerr.

Both scenarios confirm that extremality and ergoregion structure closely mirror the analogous Kerr-type solutions, preserving key causal and geometric features.

6. Observational Prospects and Distinguishability

Evaluations of thin-disk spectra and ISCO radii for rotating Cardoso black holes demonstrate that, for the high-spin regime ($C = M/a_0$7), disk observations cannot meaningfully distinguish between modified and pure Kerr spacetimes, even with the presence of a dark matter halo. Differences in disk radiative efficiency and ISCO location remain below strong observational thresholds (Heydari-Fard et al., 26 Jan 2026). For black holes with moderate spin or unusually high environmental compactness $C = M/a_0$8, deviations are more pronounced, but these configurations are astrophysically disfavored.

For multipolar scalar universes, the presence of additional parameters ($C = M/a_0$9, $$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$0, charges) does not affect horizon thermodynamics or stability but modifies asymptotic structure (such as setting the scalar universe's multipole background). Thus, potential deviations are more constrained by external field measurements than by accretion or horizon physics.

7. Summary Table: Key Metric Features

Feature	Rotating Cardoso (Halo)	Rotating Cardoso (Scalar Universe)
Environmental param.	$$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$1 (halo compactness)	$$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$2 (scalar strength), $$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$3
Metric reduction	Kerr for $$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$4	Kerr–Newman–NUT for $$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$5
ISCO shift	Mild decrease for $$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$6	Standard expressions
Radiative efficiency	$$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$7	Unchanged from Kerr–like
Horizon/ergoregion	Slightly larger $$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$8 than Kerr	Kerr–Newman–NUT structure
Thermodynamic regularity	Preserved for all $$ds^2 = g_{tt}\,dt^2 + 2g_{t\phi}\,dt\,d\phi + g_{rr}\,dr^2 + g_{\theta\theta}\,d\theta^2 + g_{\phi\phi}\,d\phi^2$$9	Preserved for all $C \to 0$0

These solutions illustrate how the rotating Cardoso black hole family generalizes Kerr physics by embedding environmental fields, with modulations of spacetime geometry that are subleading except in regimes of slow spin or high environmental density. This supports their use as testbeds for strong-field gravity and environmental matter effects.