Identifying long radio transients with accompanying X-Ray emission as disk-jet precessing black holes: The case of ASKAP J1832-0911

Aims. In this work we investigate whether the 2-min bursts every 44 min from ASKAP J1832-0911 can be explained by Lense-Thirring precession of an intermediate-mass black hole (IMBH) accretion disk launching a jet as an alternative to magnetar or white dwarf models. Methods. We derived the Lense-Thirring period $ P_\mathrm{{LT}}=\frac{\pi G M}{a c^3}r^3 $ and solved PLT = 44 min to obtain the black hole mass, M, and dimensionless radius, r = R/Rg. We estimated the equipartition field, B, at r while assuming an advection dominated accretion flow or a magnetically arrested disk accretion model; we computed the Blandford-Znajek power, PBZ,; and we compared the resulting jet luminosity to the observed radio and X-ray fluxes at D ≈ 4.5 kpc. We also describe a coherent emission model based on a merging plasmoid close to the black hole. Results. For a ∼ 0.3 − 0.9, an IMBH with M ∼ 103 − 105 M⊙ yields r ∼ 10 − 40 Rg and PLT = 44 min. Equipartition gives B ∼ 105 G at r, leading to PBZ ∼ 1035 − 39 erg s−1. With a radiative efficiency of ϵj ∼ 10−2 − 10−1, the predicted Ljet ∼ 1034 − 36 erg s−1 matches the observed FX ∼ 10−12 erg cm−2 s−1 and radio flux. The variability at ≲100 s could be clear evidence supporting this model. Conclusions. The IMBH precessing-jet model simultaneously explains the periodicity, energetics, and duty cycle of ASKAP J1832-0911. Only high time resolution X-ray timing (in order to exclude ∼s pulsations) and multi-frequency radio polarimetry (to confirm a flat, low-polarization spectrum) can definitively distinguish the IMBH model from magnetar or white dwarf scenarios.