Results 151 to 160 of about 299 (188)
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The decay of dwarf nova outbursts
Space Science Reviews, 1985Simultaneous observations at different wavelengths of the decay of dwarf-nova outbursts, show an earlier return to the quiescence level at shorter wavelengths. These observations, which show completely new aspects of outbursts, can provide strong tests for outburst models and accretion-disc theory.
H. van der Woerd, J. Heise
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Advances in Space Research, 1988
Previous papers have shown that the dwarf nova OY Car has an extensive vertical disk structure during its superoutbursts. This structure is analogous to that seen in the low mass X-ray binaries (LMXBs), in that the whole disk flares toward its edge, and there is a bulge or 'dark spot' where the mass transfer stream meets the disk edge.
T. Naylor +3 more
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Previous papers have shown that the dwarf nova OY Car has an extensive vertical disk structure during its superoutbursts. This structure is analogous to that seen in the low mass X-ray binaries (LMXBs), in that the whole disk flares toward its edge, and there is a bulge or 'dark spot' where the mass transfer stream meets the disk edge.
T. Naylor +3 more
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Astrophysics, 1999
In searchs for flare stars in the vicinity of the Pleiades cluster, three flares were detected in 1970,1972, and 1977 in a star with the coordinates α1950= 3h48m·9, δl950= 25‡15’.8. The star’s brightness at a minimum is >21m·5. The star was tentatively assigned to the U Gem type.
E. A. Parsamian +2 more
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In searchs for flare stars in the vicinity of the Pleiades cluster, three flares were detected in 1970,1972, and 1977 in a star with the coordinates α1950= 3h48m·9, δl950= 25‡15’.8. The star’s brightness at a minimum is >21m·5. The star was tentatively assigned to the U Gem type.
E. A. Parsamian +2 more
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Publications of the Astronomical Society of the Pacific, 1996
Outburst mechanisms of dwarf novae are discussed. There is a rich variety in outburst behaviors of non-magnetic cataclysmic variable stars, starting from non-outbursting nova-like stars to various sub-classes of dwarf novae (i.e., U Gem-type, Z Cam-type, and SU UMa-type).
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Outburst mechanisms of dwarf novae are discussed. There is a rich variety in outburst behaviors of non-magnetic cataclysmic variable stars, starting from non-outbursting nova-like stars to various sub-classes of dwarf novae (i.e., U Gem-type, Z Cam-type, and SU UMa-type).
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An ancient nova shell around the dwarf nova Z Camelopardalis
Nature, 2007Cataclysmic variables (classical novae and dwarf novae) are binary star systems in which a red dwarf transfers hydrogen-rich matter, by way of an accretion disk, to its white dwarf companion. In dwarf novae, an instability is believed to episodically dump much of the accretion disk onto the white dwarf.
Shara, Michael M. +15 more
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Publications of the Astronomical Society of the Pacific, 2000
We have carried out a synthetic spectral analysis of five IUE NEWSIPS archival spectra of the peculiar, very active dwarf nova CN Orionis taken at the system's lowest flux levels during quiescence. AAVSO data indicate the visual magnitude V ~ 14 for CN Ori at this time.
J. Urban +5 more
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We have carried out a synthetic spectral analysis of five IUE NEWSIPS archival spectra of the peculiar, very active dwarf nova CN Orionis taken at the system's lowest flux levels during quiescence. AAVSO data indicate the visual magnitude V ~ 14 for CN Ori at this time.
J. Urban +5 more
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Exposed white dwarfs in dwarf novae
2008Hubble Space Telescope far ultraviolet spectroscopic observations of cataclysmic variable white dwarfs, exposed during dwarf nova quiescence, have yielded a number of new insights on accretional heating, photospheric abundances of the accreted atmosphere and rotational velocities of the underlying degenerates.
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Nova and Dwarf Nova Observations with MAGIC
2016Starting in fall 2012, the MAGIC collaboration conducted a nova follow-up program in order to detect a possible VHE gamma-ray component. The program responded to Fermi-LAT detections of different types of novae at GeV energies: it initially focussed on symbiotic novae and later extended to bright Classical Novae and additional outbursts from other ...
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1985
It is now well established that the eruptions characteristic of dwarf novae result from changes in the luminosity of the accretion disc centred around the white dwarf component of these systems. These luminosity variations are most successfully accounted for by variations in the accretion flow through the disc but the mechanism responsible for this ...
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It is now well established that the eruptions characteristic of dwarf novae result from changes in the luminosity of the accretion disc centred around the white dwarf component of these systems. These luminosity variations are most successfully accounted for by variations in the accretion flow through the disc but the mechanism responsible for this ...
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Systematics of superoutbursts in dwarf novae
Astrophysics and Space Science, 1995Photometric properties of known and suspected members of the SU UMa subclass of dwarf novae are tabulated and discussed. The precessing disc model of superoutbursts gives a satisfactory quantitative explanation of the periods of superhumps and their changes during superoutburst.
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