Results 21 to 30 of about 467 (261)
Relation between Long-term Activity and Luminosity of the Pre- and Post-novae CT Ser and V446 Her
The Astronomical Journal, 2023 We show a relation of the pre- and post-nova activity of CT Ser (nova 1948) and V446 Her (nova 1960), known to have remarkably similar orbital periods P _orb . We use both photographic and CCD photometric observations.
Vojtěch Šimon
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Theory of Classical Novae [PDF]
Proceedings of The Golden Age of Cataclysmic Variables and Related Objects - III — PoS(Golden2015), 2017 We briefly review the current understanding of classical novae. Nova light curves basically exhibit a homologous nature, beside the dust blackout and oscillatory behavior, in spite of very different evolution timescale from fast to slow novae. Optically thick winds governs the evolution of decay phase of nova outbursts, of which mass-loss rate ...
Mariko Kato, Izumi Hachisu
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Symbiotic Star T CrB as an Extreme SU UMa–type Dwarf Nova
The Astrophysical Journal Letters, 2023 T CrB is a symbiotic recurrent nova that exhibits quiescent and active phases between its classical nova eruptions. The statistical properties of these active phases have been poorly studied thus far. Because of that their nature remained unknown.
Krystian Iłkiewicz +2 more
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The outbursts of classical and recurrent novae [PDF]
Astronomische Nachrichten, 2010 AbstractIn this review, I present our current state of knowledge regarding both Classical Nova and Recurrent Nova systems. Two particular objects (V1974 Cyg and RS Oph) are chosen to illustrate the range of phenomena that may be associated with their outbursts.
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The Ejecta of Classical Novae [PDF]
Symposium - International Astronomical Union, 2001 Classical novae are interacting binary stars in which a thermonuclear runaway in material accreted onto a white dwarf from a companion red dwarf results in the ejection of around 10−4M⊙ at hundreds to thousands of kilometres per second. Recent Hubble Space Telescope and MERLIN imaging of the expanding ejecta from several classical novae are presented ...
T.J. O'Brien +4 more
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The UBV Color Evolution of Classical and Symbiotic Novae
Acta Polytechnica CTU Proceedings, 2015 We identified a general course of classical nova outbursts in the B − V vs. U − B diagram. It has been reported that novae show spectra similar to A–F supergiants near optical light maximum.
I. Hachisu, M. Kato
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The Cyclic Evolution of Classical Novae [PDF]
International Astronomical Union Colloquium, 1990 The cyclic evolution of classical novae (CN) cannot be observed, as in the case of recurrent or dwarf novae. The duration of a typical cycle may range from a few thousand to a few 105 years. Thus we have to rely on theoretical studies for understanding the periodic outbursts — due to thermonuclear runaways (TNR) — on the surface of accreting white ...
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NUCLEAR MIXING METERS FOR CLASSICAL NOVAE [PDF]
The Astrophysical Journal, 2013 Classical novae are caused by mass transfer episodes from a main sequence star onto a white dwarf via Roche lobe overflow. This material forms an accretion disk around the white dwarf. Ultimately, a fraction of this material spirals in and piles up on the white dwarf surface under electron-degenerate conditions. The subsequently occurring thermonuclear
Kelly, Keegan J. +4 more
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Acta Polytechnica CTU Proceedings, 2015 Here we present the preliminary results of a project aimed at unveiling the nature of classical novae decades after their eruption. The ultimate goal of this project is to describe the population of cataclysmic variables which give rise to nova ...
A. Ederoclite +3 more
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The awakening of a classical nova from hibernation [PDF]
Nature, 2016 Cataclysmic variable stars (CVs) are close binary systems consisting of a white dwarf (primary) that is accreting matter from a low-mass companion star (secondary). From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, over $10^4$ times in brightness, occur in classical novae and are caused by a ...
Mroz, P. +11 more
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