A Persistent Black-Hole Mass Ceiling in Toroidal Scale Mechanics

Can a black hole remain arbitrarily heavy after mergers have assembled it? This paper develops the mass-ceiling prediction of Toroidal Scale Mechanics, which treats a black hole as a maintained flow structure in an underlying physical medium. The adopted intake has a mass-independent upper bound, while discharge at and above the ceiling increases with the square of the black-hole mass. Their intersection, using the theory’s committed discharge coefficient, lies at approximately one hundred billion solar masses. This coefficient supplies the numerical normalization. Above the intersection, discharge exceeds every permitted continuous intake. An exact solution gives the slowest allowed relaxation after a merger: initial masses ten and fifty percent above the ceiling fall to within one percent of it in approximately fourteen and twenty-three days, respectively. The underlying remnant study records the constant-coefficient continuation to smaller black holes as failed; that continuation requires a different state dependence. Published dynamical and joint lensing–dynamical examples reviewed here lie below the ceiling; the larger estimate for IC 1101 comes from an indirect galaxy-core relation. The decisive test is an independently confirmed black hole that persists above the calculated limit after uncertainties and the relaxation interval are accounted for. Such an object rejects the specified intake–discharge construction.