The sustained post-outburst brightness of Nova Per 2018, the evolved companion, and the long orbital period

TL;DR

The paper studies Nova Per 2018's long-lasting brightness plateau, characterizing its companion star, orbital period, and ejecta composition, revealing a massive white dwarf and a system bridging classical and symbiotic novae.

Contribution

It provides the first detailed characterization of Nova Per 2018 during its plateau phase, including orbital period, companion star type, and ejecta composition, linking classical and symbiotic nova properties.

Findings

Orbital period of 3.4118 days, the longest for a classical nova.

Companion star identified as G9 IV/III, 3.6 Gyr old.

Ejecta show a huge Ne overabundance, indicating a massive white dwarf.

Abstract

Nova Per 2018 (= V392 Per) halted the decline from maximum when it was 2mag brighter than quiescence and since 2019 has been stable at such a plateau. The ejecta have already fully diluted into the interstellar space. We obtained BVRIgrizY photometry and optical spectroscopy of V392 Per during the plateau phase and compared it with equivalent data gathered prior to the nova outburst. We find the companion star to be a G9 IV/III and the orbital period to be 3.4118 days, making V392 Per the longest known period for a classical nova. The location of V392 Per on the theoretical isochrones is intermediate between that of classical novae and novae erupting within symbiotic binaries, in a sense bridging the gap. The reddening is derived to be E(B-V)=0.72 and the fitting to isochrones returns a 3.6 Gyr age for the system and 1.35 Msun, 5.3 Rsun, and 15 Lsun for the companion. The huge Ne overabundance in the ejecta and the very fast decline from nova maximum both point to a massive white dwarf (M(WD) >= 1.1-1.2 Msun). The system is viewed close to pole-on conditions and the current plateau phase is caused by irradiation of the CS by the WD still burning at the surface.