Identification of recurrent novae from parametric modeling of the optical light curve

Abstract

Novae, characterized by sudden brightening in binary star systems, are categorized into classical novae (CNe) and recurrent novae (RNe) based on their recurrence timescales. However, identifying RNe, which occur within 100 years, presents observational challenges. A reasonable signature of RNe has been theorized and statistically validated to address this -- the presence of a plateau in the optical light curve. Among the known RNe, except T CrB and V3890 Sgr displaying S-class light curve, the rest 9 out of 11 have a P-class light curve. But classical novae can also present plateaus, which further complicates the problem of distinguishing CNe from RNe just based on plateau. Hence, in this study, we aim to conduct a phenomenological analysis of P-class light curves to comment on the recurrence nature of novae. We utilize data primarily from the AAVSO database and identify a parameter space to represent all P-class light curves, anticipating distinct parameter distributions for CNe and RNe. Analysis of parameter distributions successfully distinguishes RNe from CNe and reveals potential connections with white dwarf mass and mass accretion rate, which are the key factors. Our method indicates KT Eri to be a recurrent nova, consistent with a recent study, despite only one observed outburst. The analysis also indicates the possibility of recurrence for V2860 Ori, a prediction that may be tested by deep search for nova super-remnant for this source. Our method demonstrates the feasibility of distinguishing P-class classical and recurrent novae based solely on the optical light curve. As observations of new novae increase, this method holds promise for more precise predictions of nova recurrence nature in the future.