Symbiotic novae are slow irregular eruptive variable stars with very slow nova-like outbursts with an amplitude of between 9 and 11 magnitudes. The symbiotic nova remains at maximum for one or a few decades, and then declines towards its original luminosity. Variables of this type are double star systems with one red giant, which probably is a Mira variable, and one white dwarf, with markedly contrasting spectra and whose proximity and mass characteristics indicate it as a symbiotic star. The red giant fills its Roche lobe so that matter is transferred to the white dwarf and accumulates until a nova-like outburst occurs, caused by ignition of thermonuclear fusion. The temperature at maximum is estimated to rise up to 200,000 K, similar to the energy source of novae, but dissimilar to the dwarf novae. The slow luminosity increase would then be simply due to time needed for growth of the ionization front in the outburst.
- Bryan, Greg L.; Kwok, Sun (1991). "Energy distributions of symbiotic novae". The Astrophysical Journal. 368: 252–260. Bibcode:1991ApJ...368..252B. doi:10.1086/169688.
- MURSET U.; NUSSBAUMER H. (1994). "Temperatures and luminosities of symbiotic novae". Astronomy & Astrophysics. 282: 586–604. Bibcode:1994A&A...282..586M.
- Photometric and Spectroscopic Evolution of the Symbiotic Nova ...