Tidal Heating Rates and Surface Heat Flow for Eccentric Exomoons

This paper computes a quantitative budget for one aspect of exomoon physics: the subject stated in the title, evaluated from stated assumptions with every number produced by the deposited calculation. Headline results are io_heating_TW = 44.1; io_heat_flow_W_m2 = 1.06; earthmoon_e005_TW = 65567.8; enceladus_TW = 0.009. Tides raised inside a moon by its planet flex the interior once per orbit whenever the orbit is eccentric or the spin is not perfectly synchronous, and the flexing dissipates energy as heat. On Io that dissipation drives the most vigorous volcanism in the Solar System; on Europa and Enceladus it maintains subsurface oceans beneath ice shells. For an exomoon the same physics is a detection channel The results are compared with published Solar System values and with the constraints attached to reported exomoon candidates where those apply, and the conditions under which the computed budget would change are stated explicitly. Computed from stated assumptions, not measured.