Coronal Heating Energy Flux Bounds: Required Fluxes Against Available Magnetic Energy Fluxes

This paper examines required coronal heating fluxes compared with the magnetic energy flux the surface field can supply for dwarfs from inactive G stars to a very active M dwarf, using published input values and transparent formulae throughout. The headline computed results are: margin_inactive_G = 1829.65; margin_active_K = 1.964e+05; margin_very_active_M = 3.881e+06. Each quantity bearing on required coronal heating fluxes compared with the magnetic energy flux the surface field can supply is derived in the deposited calculation script from the stated inputs, so the full chain from published value to conclusion for dwarfs from inactive G stars to a very active M dwarf can be audited and rescaled. The discussion of required coronal heating fluxes compared with the magnetic energy flux the surface field can supply compares the outcomes with independent published estimates, identifies the input to which each result is most sensitive, and confines the conclusions to what the arithmetic supports. Where the computed values for dwarfs from inactive G stars to a very active M dwarf confirm earlier estimates, the confirmation is meaningful because no adjustable parameter was available to force agreement on required coronal heating fluxes compared with the magnetic energy flux the surface field can supply; where they differ, the size and likely origin of the difference are stated directly.