Results 21 to 30 of about 299 (188)
AT Cnc: A SECOND DWARF NOVA WITH A CLASSICAL NOVA SHELL [PDF]
The Astrophysical Journal, 2012 We are systematically surveying all known and suspected Z Cam-type dwarf novae for classical nova shells. This survey is motivated by the discovery of the largest known classical nova shell, which surrounds the archetypal dwarf nova Z Camelopardalis.
Shara, Michael M. +7 more
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Temperatture esttiimattiion off EXDRA and SSUMI dwarff Nova systtems from spectroscopic data
Iraqi Journal of Physics, 2019 The seasonal behavior of the light curve for selected star SS UMI and EXDRA during outburst cycle is studied. This behavior describes maximum temperature of outburst in dwarf nova.
Arshed Ali Kadhem
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Dwarf nova outbursts with magnetorotational turbulence [PDF]
Monthly Notices of the Royal Astronomical Society, 2016 The phenomenological Disc Instability Model has been successful in reproducing the observed light curves of dwarf nova outbursts by invoking an enhanced Shakura-Sunyaev $α$ parameter $\sim0.1-0.2$ in outburst compared to a low value $\sim0.01$ in quiescence.
Coleman, M. S. B. +4 more
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Outbursts of dwarf novae [PDF]
Publications of the Astronomical Society of the Pacific, 1984 A review is given of the observational facts related to the outbursts of dwarf novae and of relevant aspects of the theory of accretion disks. It now appears possible to explain the outbursts of dwarf novae in terms of a nonstationary accretion behavior. Between the outbursts, the material supplied by the secondary component is stored in the relatively
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The Astrophysical Journal, 1983 Observational data on mass-transfer rates and radii of disks indicate that the outer parts of disks in novae and nova-like binaries are sufficiently hot for stationary accretion; those in dwarf novae are too cool to avoid an accretion instability, while these in Z Cam systems are the borderline cases.
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Symposium - International Astronomical Union, 1976 Recent work on the physical processes resulting from mass transfer between the red and blue components of dwarf nova binaries is reviewed. The optical behaviour of the blue component's accretion disc suggests that it may be the infall, accretion energy which is being liberated during outbursts.
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THE DWARF NOVA OUTBURSTS OF NOVA HER 1960 (=V446 HER) [PDF]
The Astronomical Journal, 2011 To appear at the Astronomical Journal; 7 pages, 1 table, 11 ...
Honeycutt, R. K. +2 more
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OGLE-BLG504.12.201843: a possible extreme dwarf nova
Monthly Notices of the Royal Astronomical Society, 2022 ABSTRACT We present the analysis of existing optical photometry and new optical spectroscopy of the candidate cataclysmic variable star OGLE-BLG504.12.201843. As was shown previously, this object has an orbital period of 0.523419 d and exhibits year-long outbursts with a mean period of 973 d.
Camille Landri +7 more
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V2487 Oph 1998: a post nova in an intermediate polar
EPJ Web of Conferences, 2014 V2487 Oph (Nova Oph 1998) is a classical nova that exploded in 1998. XMM-Newton observations performed between 2 and 9 years after the explosion showed emission related to restablished accretion, and indicative of a magnetic white dwarf.
Hernanz Margarita
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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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