The slow decline of the Galactic recurrent novae T Pyxidis, IM Normae, and CI Aquilae
arXiv:1502.06763 · doi:10.1093/mnras/stv265
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.
References in corpus (17)
- The NextGen Model Atmosphere grid for $3000\le \Teff \le 10000\K$
- Comprehensive Photometric Histories of All Known Galactic Recurrent Novae
- Catalog of 93 Nova Light Curves: Classification and Properties
- Swift X-Ray Observations of Classical Novae. II. The Super Soft Source sample
- X-ray emission from classical and recurrent-novae observed with ROSAT
- The Evolution of Nova V382 Vel 1999
- The Nova Shell and Evolution of the Recurrent Nova T Pyxidis
- The orbital period and system parameters of the recurrent nova T Pyx
- The secrets of T Pyxidis II. A recurrent nova that will not become a SN Ia
- The 2011 Outburst of Recurrent Nova T Pyx: X-ray Observations Expose the White Dwarf Mass and Ejection Dynamics
- The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst. II.The optically thin phase and the structure of the ejecta in recurrent novae
- Revised analysis of the supersoft X-ray phase, helium enrichment, and turn-off time in the 2000 outburst of recurrent nova CI Aquilae
- The 2011 Outburst of Recurrent Nova T Pyx: Radio Observations Reveal the Ejecta Mass and Hint at Complex Mass Loss
- Morpho-Kinematical Modelling of Nova Eridani 2009 (KT Eri)
- XMM-Newton observations of Nova LMC 2000
- Non-Equipartition of Energy, Masses of Nova Ejecta, and Type Ia Supernovae
- Hubble Space Telescope Far Ultraviolet Spectroscopy of the Recurrent Nova T Pyxidis