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The nova type outburst of the symbiotic star AS 296

International Astronomical Union Colloquium, 1990
AbstractThe photometric and spectroscopic evolutions, displayed by AS 296 since the June 1988 outburst ([1]), are presented and discussed. The main features of the model outlined by [2], [3] and [4], are confirmed and further developped. An orbital period of about 3 years is inferred from Hα modulation (see [5]).The outburst originated from a TNR event
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The Slow Nova RR Tel and the Symbiotic Stars

1977
The slow nova RR Tel belongs to a group of symbiotic stars which contain in addition to an M type component, a hot dust shell. For symbiotics without dust, infrared photometry shows that the M component is constant in light. For these systems the mass exchange is usually considered to be through the inner Lagrangian point.
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Photoionization Modelling of Quiescence-Phase Spectra of Novae and a Symbiotic Star

Monthly Notices of the Royal Astronomical Society, 2020
Ramkrishna Das   +2 more
exaly  

Recurrent and Symbiotic Novae in Data From the Optical Gravitational Lensing Experiment

Monthly Notices of the Royal Astronomical Society, 2014
Przemek Mroz   +2 more
exaly  

On the Late-Type Components of Slow Novae and Symbiotic Stars

Monthly Notices of the Royal Astronomical Society, 1980
David A Allen
exaly  

On the new minimum of the symbiotic nova PU Vulpeculae

Monthly Notices of the Royal Astronomical Society, 1995
E. A. Kolotilov, U. Munari, B. F. Yudin
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