The slow decline of the Galactic recurrent novae T Pyxidis, IM Normae, and CI Aquilae

TL;DR

This paper investigates why certain Galactic recurrent novae with short orbital periods have unusually long optical decline times, proposing that retained material within the Roche lobe delays ionization and extends the decline.

Contribution

It introduces a new explanation for the slow optical decline in specific recurrent novae, emphasizing the role of retained transferred material within the Roche lobe.

Findings

Retained material within the Roche lobe delays ejecta ionization.

High mass transfer rates and short orbital periods favor this phenomenon.

A schematic model supports the scenario quantitatively.

Abstract

A distinguishing trait of the three known Galactic recurrent novae with the shortest orbital periods, T Pyx, IM Nor, and CI Aql, is that their optical decline time-scales are significantly longer than those of the other recurrent systems. On the other hand, some estimates of the mass of the ejecta, the velocity of the ejecta, and the duration of the soft X-rays emission of these systems are of the order of those of the other recurrent systems and the fast classical novae. We put forth a tentative explanation of this phenomenon. We propose that in these systems part of the material transferred from the companion during the first few days of the eruption remains within the Roche lobe of the white dwarf, preventing the radiation from ionizing the ejecta of the system and increasing the optical decline time-scale. We explain why this phenomenon is more likely in systems with a high mass transfer rate and a short orbital period. Finally, we present a schematic model that shows that the material transferred from the companion is sufficient to absorb the radiation from the white dwarf in these systems, ultimately supporting this scenario as quantitatively realistic.