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 Blandford-Znajek jet, as an alternative to magnetar or white-dwarf models. Methods: We derive the Lense-Thirring period $P_{\mathrm{L}\mathrm{T}}=\frac{\pi GM}{a{c}^3}{r}^3$ and solve $P_{\mathrm{L}\mathrm{T}}=44$ min for black-hole mass M and dimensionless radius $r=R\mathrm{/}{R}_g$. We estimate the equipartition field B at r, compute the Blandford-Znajek power $P_{\mathrm{B}\mathrm{Z}}$, and the power expected from a gap at the black hole magnetosphere, and compare the resulting jet luminosity to the observed radio and X-ray fluxes at $D\approx 4.5$ kpc. We also evaluate expected high-frequency variability and the angular size for Very Long Baseline Interferometry (VLBI) observations. Results: For $a\sim 0.3\text{\hspace{0.17em}⁣}-\text{\hspace{0.17em}⁣}0.9$, an IMBH with $M\sim {10}^3\text{\hspace{0.17em}⁣}-\text{\hspace{0.17em}⁣}{10}^5{M}_{\odot }$ yields $r\sim 10\text{\hspace{0.17em}⁣}-\text{\hspace{0.17em}⁣}40R_g$ and $P_{\mathrm{L}\mathrm{T}}=44$ min. Equipartition gives $B\sim {10}^5$ G at r, leading to $P_{\mathrm{B}\mathrm{Z}}\sim {10}^{35\text{\hspace{0.17em}⁣}-\text{\hspace{0.17em}⁣}39}$ erg ${\mathrm{s}}^{-1}$. With radiative efficiency ${\epsilon }_j\sim {10}^{-2}\text{\hspace{0.17em}⁣}-\text{\hspace{0.17em}⁣}{10}^{-1}$, the predicted $L_{\mathrm{j}\mathrm{e}\mathrm{t}}\sim {10}^{34\text{\hspace{0.17em}⁣}-\text{\hspace{0.17em}⁣}36}$ erg ${\mathrm{s}}^{-1}$ matches the observed $F_X\sim {10}^{-12}$ erg $\mathrm{c}{\mathrm{m}}^{-2}$ ${\mathrm{s}}^{-1}$ and radio flux, variability on $\lesssim 100$ s could be a smoking gun of 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 (to check $\sim$s pulsations) and multi-frequency radio polarimetry can definitively distinguish it from magnetar or white-dwarf scenarios.