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

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.

Hubble Space Telescope Far-UV Spectroscopy of the Short Orbital Period Recurrent Nova CI Aql: Implications for White Dwarf Mass Evolution

“…However, estimates of their ejecta masses, ejection velocities and soft-X-ray runoff times are comparable to other recurrent novae and fast classical novae. This led Caleo & Shore (2015) to propose that their slower optical declines can be explained as gas which is transferred into the Roche lobe of the WD by the donor star in the first few days of the nova explosion, blocking the radiation from ionizing the ejecta and increasing the optical decline timescale. Whether or not this explains their distinctive slow declines requires further exploration.…”