IMBH Spin Constraint Synthesizer

Four independent spin-constraint methods for OC's IMBH — QPO resonance, BZ radio upper bound, superradiance spin-down, and LISA ringdown — synthesized into a joint (mass, spin) posterior grid. Highlights the BZ-efficient regime where MTH engineering becomes viable.

🔬 Multi-method constraints
Global Parameters
8,200 M☉
Schwarzschild radius rsAU
Eddington luminosityW
BZ-viable spin thresholda★ ≥ 0.5
MTH-optimal spin thresholda★ ≥ 0.9
Method Inputs — Toggle active constraints
QPO Resonance
Török et al. 3:2 epicyclic model
3.0 mHz
a★ ≈ —
BZ Radio Limit
Radio non-detection → P_BZ upper bound
10⁻⁸
a★ ≤ —
Superradiance
Ultra-light boson spin-down constraint
10⁻¹⁴·² eV
Spin-down: —
LISA Ringdown
IMRI merger ringdown — spin from QNM frequencies. LISA sensitivity below 0.1 Hz; OC IMRI detectable if mass ratio q > 10⁻³.
LISA verdict: —
Joint (Mass, Spin) Posterior Grid

Grid shading: Ruled out by ≥1 active constraint  |  Marginal  |  Allowed by all active constraints  |  BZ-optimal zone (a★≥0.9)

Spin a★ (x) × Mass log₁₀(M_BH/M☉) (y)
Allowed spin range (active constraints)
MTH viability (a★ ≥ 0.9)
BZ power at a★=0.9 (B=10⁶ T)W

QPO resonance (Török et al. 2011)

The 3:2 parametric epicyclic resonance model predicts QPO frequencies ν_U and ν_L from ISCO orbital frequencies: ν_U = ν_K(r_res) and ν_L = ν_K/2, where r_res depends on spin. For a given observed ν_U, the spin is determined by inverting this relation. No QPO has been detected in OC's IMBH yet; the slider sets a hypothetical future detection.

BZ radio upper bound

The Blandford–Znajek (1977) jet power P_BZ ∝ B² M² a². The radio luminosity of a jet scales as L_R ∝ P_BZ^α (α ~ 0.7). Given a radio upper limit, this sets an upper bound on a★ (assuming a fiducial magnetic field B at the horizon). At OC's current radio non-detection level (~10⁻⁸ W/Hz), the BZ spin constraint is weak unless B is constrained.

Superradiance

Rotating black holes can transfer angular momentum to ultralight boson fields if the Compton wavelength matches the gravitational radius: m_b c² / ℏ ≈ GM/c³ × 2π. For OC's IMBH (~10⁴ M☉), the resonant boson mass is ~5.6×10⁻¹⁵ eV (10⁻¹⁸ eV corresponds to SMBH-scale BHs of ~10⁶–10⁷ M☉). If such bosons exist (ALP dark matter), superradiance would have spun down the BH on a timescale much shorter than OC's age — implying either a low spin or no such boson at that mass.

LISA ringdown

A compact object (neutron star or stellar BH) inspiraling into OC's IMBH produces quasi-normal mode (QNM) ringdown that encodes the spin. The dominant (l=m=2) QNM frequency scales as f_QNM ≈ c³/(2πGM) × 0.37 (1 − 0.23 a★) for near-Schwarzschild. LISA sensitivity at ~mHz covers this for an IMBH at OC's distance if mass ratio q > 10⁻³.

References

Török et al. 2011 (A&A 531:A59) · Blandford & Znajek 1977 (MNRAS 179:433) · Arvanitaki & Dubovsky 2011 (PRD 83:044026) · Amaro-Seoane 2022 (Living Reviews in Relativity)