The Dvali-Osmanov Signal Chain

A Phase 5 OCS civilisation operates kugelblitz computers — black holes formed from focused radiation, which evaporate via Hawking radiation and emit particles democratically across all Standard Model species. The neutrino channel is particularly valuable: neutrinos escape the IMBH accretion environment without absorption, unlike photons. Dvali & Osmanov (2023) showed that for kugelblitz with T_Hawking >> 1 GeV, approximately 45% of total Hawking power is emitted as neutrinos. At M = 10&sup8; kg (Scenario A), T_H ≈ 10¹⁵ K and total Hawking power ≈ 1.6×10¹⁴ W. At M = 10¹⁰ kg (Scenario B), T_H ≈ 10¹³ K and Hawking power ≈ 1.6×10¹⁰ W — but the longer evaporation time of ~10&sup8; years makes it a viable persistent signal source.

The neutrino flux from OC depends on total emitted power and the inverse-square law. A 10&sup8; kg kugelblitz emits ~1.6×10¹⁴ W total Hawking power, of which ~7.2×10¹³ W is neutrinos. At 5.49 kpc, the isotropic flux is ~2.5×10−²⁸ GeV/cm²/s — 16 orders of magnitude below current IceCube sensitivity. A detectable signal would require ~10¹⁰ simultaneous kugelblitz, or a single much smaller one (M ~ 1 tonne) with t_evap ~ seconds. This tool lets you explore the detectability landscape by varying kugelblitz count, mass, and distance. The key result: the neutrino flux is real but buried, and only a large-scale coordinated fleet or a dedicated tonne-scale kugelblitz burst would cross the IceCube threshold.

A multi-messenger detection of the kugelblitz signal requires simultaneous excesses in the neutrino, gamma-ray, and possibly gravitational-wave channels. For the Dvali-Osmanov scenario, the primary channel is neutrino — but an OC-direction neutrino excess would trigger follow-up in Fermi-LAT (gamma-ray MSP background check) and MeerKAT (radio). The false-alarm probability from a single-channel detection is unacceptably high; the multi-messenger requirement raises the bar but also provides strong circumstantial evidence if multiple channels register simultaneously. A tonne-scale kugelblitz evaporating over seconds would also produce a gravitational-wave burst detectable by LIGO within ~0.1 pc. The multi-messenger alert tool maps the detection thresholds across all channels as a function of source distance and power.