Results 41 to 50 of about 125,367 (265)
International Astronomical Union Colloquium, 1979 AbstractExtensive photoelectric observations of EX Hya were obtained between 1962 and 1976 at different telescopes and observatories. Evaluation of the data reveals a decrease of the orbital period at the rate Ṗ = −5.2 × 10−12. This period change is likely caused by mass transfer with angular momentum exchange between orbital motion and disc rotation ...
N. Vogt, W. Krzeminski, C. Sterken
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Observations of Eclipsing Dwarf Novae [PDF]
International Astronomical Union Colloquium, 1987 AbstractHigh Speed Photometry of four eclipsing dwarf novae, Z Cha, OY Car, HT Cas and IP Peg, is used to determine the orbital parameters and the masses of the two stars in each system. The mass ratio, q, and inclination, i, are found by constraining theoretical stream trajectories (Lubow and Shu 1975) to pass through the observed light centre of the ...
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Statistical properties of dwarf novae-type cataclysmic variables: the outburst catalogue [PDF]
, 2015 The outburst catalogue contains a wide variety of observational properties for 722 dwarf nova (DN)-type cataclysmic variables (CVs) and 309 CVs of other types from the Catalina Real-time Transient Survey.
D. Coppejans +7 more
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The Temperatures of White Dwarfs in Dwarf Novae [PDF]
International Astronomical Union Colloquium, 1996 AbstractWe attempt to measure the temperature of all the quiescent dwarf novae that have been observed with IUE, by fitting the observed flux distribution of white dwarfs (WDs) with known temperatures. This approach gives results similar to those using much more sophisticated modelling, but allows us to investigate the relationship with system ...
B. J. M. Hassall, C. La Dous
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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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When does an old nova become a dwarf nova? Kinematics and age of the nova shell of the dwarf nova AT Cancri [PDF]
Monthly Notices of the Royal Astronomical Society, 2016 8 pages, 8 ...
Shara, Michael M. +4 more
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Modeling the EUV spectra of optically thick boundary layers of dwarf novae in outburst [PDF]
, 2014 Here we compute detailed model spectra of recently published optically thick one-dimensional radial baundary layer (BL) models in cataclysmic variables and compare them with observed soft X-ray/extreme ultraviolet (EUV) spectra of dwarf novae in outburst.
V. Suleimanov +3 more
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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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Analysis of Three SU UMa-Type Dwarf Novae in the Kepler Field [PDF]
, 2013 We studied the Kepler light curves of three SU UMa-type dwarf novae. Both the background dwarf nova of KIC 4378554 and V516 Lyr showed a combination of precursor-main superoutburst, during which superhumps always developed on the fading branch of the ...
Taichi Kato, Y. Osaki
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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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