Do novae have optically thick winds during outburst with large deviations from spherical symmetry?

TL;DR

This paper investigates whether optically thick winds occur during nova outbursts, especially considering deviations from spherical symmetry, and discusses how magnetic fields might influence wind behavior and observed variations.

Contribution

It proposes that large deviations from spherical symmetry, possibly caused by magnetic fields, can explain early phase variations in nova outbursts, challenging previous assumptions.

Findings

Optically thick winds are likely present in early nova stages.

Deviations from spherical symmetry can account for phase-dependent variations.

Magnetic fields may significantly influence nova wind structures.

Abstract

The evidence for the presence of optically thick winds, produced by classical novae after optical maximum, has been challenged in recent papers. In addition, signs of orbital phase dependent photometric variations, sometimes seen quite early in the development of nova outbursts, are hard to interpret in the framework of optically thick envelopes and especially winds. A general discussion for belief in the presence of optically thick winds with increasing ejection velocities during the early stages of novae after their explosion, must be given. This has to be done in order to clarify ideas about novae as well as to contribute in particular to the understanding of the behaviour of novae V1500 Cyg and V1493 Aql showing phase dependent variations during very early decline after the outburst. Possible ways of overcoming the apparent contradiction of phase dependent variations through the production of deviations from spherical symmetry of the winds, are looked at and order of magnitude estimates are made for different theoretical scenarios, which might produce such deviations. It is found that large deviations from spherical symmetry of the optically thick winds in early phases after the explosion can easily explain the problem of variations. In particular, the presence of a magnetic field might have had a non-negligible effect on the wind of V1500 Cyg, while at the present there is not enough information available concerning V1493 Aql. Optically thick winds/envelopes are almost certainly present in the early stages after optical maximum of a nova, while it is difficult to make pure Hubble flow models fit the observations of those stages. New more detailed observational and theoretical work, in particular including the effects of magnetic fields on the winds, is needed.