Spatio-kinematic models of five nova remnants: correlations between nova shell axial ratio, expansion velocity, and speed class

TL;DR

This study models five nova remnants to explore how their 3D shapes relate to expansion velocity and decline time, revealing correlations that support theories on nova ejecta interactions and white dwarf properties.

Contribution

It provides detailed 3D morpho-kinematic models of five nova shells and establishes correlations between their shape, expansion velocity, and decline time, confirming theoretical predictions.

Findings

Fastest novae have the smallest axial ratios.

Nova shell HRDel's high velocity contradicts its long decline time.

Ellipsoidal nova remnants show anti-correlation between velocity and axial ratio.

Abstract

We present long-slit intermediate-dispersion spectroscopic observations and narrow-band direct imaging of four classical nova shells, namely TAur, HRDel, DQHer and QUVul, and the nova-like source CKVul. These are used to construct models of their nebular remnants using the morpho-kinematic modelling tool Shape to reveal their 3D shape. All these nova remnants but CKVul can be described by prolate ellipsoidal shells with different eccentricity degree, from the spherical QUVul to the highly elongated shell with an equatorial component HRDel. On the other hand, CKVul shows a more complex structure, with two pairs of nested bipolar lobes. The spatio-kinematic properties of the ellipsoidal nova shells derived from our models include their true axial ratios. This parameter is expected to correlate with the expansion velocity and decline time C3 (i.e., their speed class) of a nova as the result the interaction of the ejecta with the circumstellar material and rotation speed and magnetic field of the white dwarf. We have compared these three parameters including data available in the literature for another two nova shells, V533 Her and FH Ser. There is an anti-correlation between the expansion velocity and the axial ratio and decline time C3 for nova remnants with ellipsoidal morphology, and a correlation between their axial ratios and decline times C3, confirming theoretical expectations that the fastest expanding novae have the smallest axial ratios. We note that the high expansion velocity of the nova shell HRDel of 615 km/s is inconsistent with its long decline time C3 of 250 days.