Photometric evolution, orbital modulation and progenitor of Nova Mon 2012

TL;DR

This study provides detailed optical lightcurves and spectral analysis of Nova Mon 2012, revealing its orbital modulation, progenitor characteristics, and evolution through the super-soft X-ray phase, offering insights into its binary system and eruption behavior.

Contribution

It offers the first densely mapped lightcurves of Nova Mon 2012, constrains the progenitor system, and interprets the orbital modulation in the context of binary star interactions.

Findings

Orbital period of 0.29585 days with sinusoidal modulation.

Progenitor system includes a K3V star at 1.5 kpc distance.

Optical lightcurves show smooth evolution and phase-specific features.

Abstract

We present and discuss accurate and densely mapped BVRI lightcurves of the neon Nova Mon 2012, supplemented by the evolution in Stromgren b and y bands and in the integrated flux of relevant emission lines. Our monitoring started with the optical discovery of the nova and extend to day +270, well past the end of the super-soft phase in X-rays. The nova displayed very smoothly evolving lightcurves. A bifurcation between y and V light-curves took place at the start of the SSS phase, and a knee developed toward the end of the SSS phase. The apparent magnitude of the nova at the unobserved optical maximum is constrained to +2.8=<V=<4.2. The appearance, grow in amplitude and then demise of a 0.29585 (+/-0.00002) days orbital modulation of the optical brightness was followed along the nova evolution. The observed modulation has a near-sinusoidal shape and a weak secondary minimum at phase 0.5. We favor an interpretation in terms of super-imposed ellipsoidal distortion of the Roche lobe filling companion and irradiation of its side facing the WD. Similar lightcurves are typical of symbiotic stars where a Roche lobe filling giant is irradiated by a very hot WD. Given the high orbital inclination, mutual occultation between the donor star and the accretion disk could contribute to the observed modulation. The optical+infrared spectral energy distribution of Nova Mon 2012 during the quiescence preceeding the outburst is nicely fitted by a early K-type main-sequence star (~K3V) at 1.5 kpc distance, reddened by E(B-V)=0.38, with a WD companion and an accretion disk contributing to the observed blue excess and moderate Halpha emission. A typical early K-type main-sequence star with a mass of ~0.75 Msun and a radius of ~0.8 Rsun, would fill its Roche lobe for a P=0.29585 day orbital period and a more massive WD companion.