The most prominent visual feature within Inverness Corona is the bright "chevron" located within its core region, representing the largest observed high-albedo unit on Miranda.

[2]: 6  Due to Inverness Corona's youth, its features exceptionally pristine, with a team of planetary scientists led by Michelle R. Kirchoff evaluating it as the least degraded terrain unit observed on Miranda.

Two primary models of coronae formation have arisen since the Voyager 2 flyby: thermally- or compositionally-driven upwelling of material that drives tectonic extension and/or cryovolcanism, or downwelling due to impact events or reaccretion.

A team of planetary scientists led by Erin J. Leonard additionally proposed ice-shell thickening as a potential alternative to the two.

[9] This interpretation was corroborated by R. Greenberg and collaborators in 1991, who viewed the concentric banding of Inverness as being controlled by the layout of arcuate eruptive vents.

[4]: 730  However, Erin J. Leonard and collaborators disfavored a cryovolcanic interpretation, noting the lack of observable flow features in Voyager 2 imagery and associating Inverness Corona's bright material as impact ejecta.

"Sinker tectonics", proposed by D. M. Janes and H. J. Melosh in 1988, is also unlikely to be responsible for the formation of Inverness Corona due to the lack of observed thrust faults associated with material sinking in Miranda's interior.

[2]: 6 Alternatively, Erin J. Leonard and collaborators proposed in 2023 that ice shell thickening could explain the formation of Inverness Corona.