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

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