An Extended Grid of Nova Models. III. Very Luminous, Red Novae
Michael M. Shara, Ofer Yaron, Dina Prialnik, Attay Kovetz, David, Zurek

TL;DR
This study extends nova models to explain very luminous, red eruptions, predicting observable differences from star merger events, including a fast-fading hot white dwarf remnant and specific luminosity evolution.
Contribution
It demonstrates that classical nova models can produce extremely luminous, red eruptions in a specific parameter space, contrasting with star merger models and predicting observable post-eruption behaviors.
Findings
Novae can reach luminosities of 10^7 Lsun.
Remnant white dwarf will fade within decades.
Ejecta become redder over time.
Abstract
Extremely luminous, red eruptive variables like RV in M31 are being suggested as exemplars of a new class of astrophysical object. Our greatly extended series of nova simulations shows that classical nova models can produce very red, luminous eruptions. In a poorly studied corner of 3-D nova parameter space (very cold, low-mass white dwarfs, accreting at very low rates) we find bona fide classical novae that are very luminous and red because they eject very slowly moving, massive envelopes. A crucial prediction of these nova models - in contrast to the predictions of merging star ("mergeburst") models - is that a hot remnant, the underlying white dwarf, will emerge after the massive ejected envelope has expanded enough to become optically thin. This blue remnant must fade on a timescale of decades - much faster than a "mergeburst", which must fade on timescales of millennia or longer.…
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