  A nova super-remnant (NSR) is an immense structure associated with a nova
that forms when frequent and recurrent nova eruptions sweep up surrounding
interstellar material (ISM) into a high density and distant shell. The
prototypical NSR, measuring over 100 pc across, was discovered in 2014 around
the annually erupting nova M31N 2008-12a. Hydrodynamical simulations
demonstrated that the creation of a dynamic NSR by repeated eruptions
transporting large quantities of ISM is not only feasible but that these
structures should exist around all novae, whether the white dwarf (WD) is
increasing or decreasing in mass. But it is only the recurrent nova (RNe) with
the highest WD masses and accretion rates that should host observable NSRs. KT
Eridani is, potentially, the eleventh RNe recorded in the Galaxy and is also
surrounded by a recently unveiled H{\alpha} shell tens of parsecs across,
consistent with a NSR. Through modelling the nova ejecta from KT Eri, we
demonstrate that such an observable NSR could form in approximately 50,000
years, which fits with the proper motion history of the nova. We compute the
expected H{\alpha} emission from the KT Eri NSR and predict that the structure
might be accessible to wide-field X-ray facilities.
