The event horizon's edge is never calm. Quantum vacuum boils there, and particles sometimes burst out of this foam: that is how Stephen Hawking in 1974 discovered black hole radiation, forever linking gravity with quantum field theory. But for a long time, calculations covered only massless and simplest massive fields. The real particles of nature, W and Z bosons of the Standard Model, require a Proca field description, and its behavior in a rotating black hole geometry remained a mystery. Yet such fields are precisely what should be born during the evaporation of primordial black holes — tiny asteroid-mass objects living their last moments somewhere in our Galaxy.

A group of physicists closed this gap by conducting a large-scale numerical simulation of the Proca field equations in Kerr spacetime curvature. The key to the puzzle is three polarization modes. Their behavior resembles a jazz trio, with the black hole's rotation acting as conductor. The scalar mode (S=+1) is a deep double bass setting the rhythm at slow rotation; it is strong while the hole is lazy. The first vector mode (S=-1) is a solo violin capable of superradiance: the wave steals rotational energy and soars up if the condition \( \omega < m\Omega_H \) is met — the particle must spin slower than the hole itself. The second vector mode (S=0) is a viola, modest and almost invisible.

The most striking result concerns particle mass. In old scenarios, if the hole's temperature was low, the birth of heavy fragments could be forgotten. Rotation overturns this logic. Calculations showed: at near-extremal spin, the emission spectrum shifts to such high energies that particles with mass one hundred times the Hawking temperature leave the horizon without much trouble. It is like a storm that lifts not dust but stones — energy is drawn from the rotation reserve. The scalar mode, conversely, quickly fades with increasing mass, losing two orders of magnitude in intensity. The three voices sound completely different.

This polyphony matters for the search for primordial black holes. Their typical mass, about 10¹⁵ grams, means evaporation should produce gamma-ray bursts accessible to Fermi-LAT and neutrino detectors like IceCube. Without accurate spectra of all polarizations, we risk missing the signal or confusing it with noise. Moreover, in the complex balance of entropy, first conceptualized by Jacob Bekenstein, and angular momentum, each mode plays its role: vector waves carry away rotation more efficiently, changing the hole's fate. Understanding this trio is a step toward the complete life story of a black hole, from quantum birth to final flash.

Every particle torn from the boiling vacuum at the horizon turns out to be sung in three voices. The polarization trio is not an abstraction but a key to the score of dying black holes. The next act, include all Standard Model fields in the code, to hear the full symphony.