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The Orophilous Shrubby Vegetation of the Juniperetalia hemisphaericae Order in Sicily: A Refuge Habitat for Many Endemic Vascular Species. [PDF]
Plants (Basel)Sciandrello S, Giusso Del Galdo G.
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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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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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Nova Scorpius 1437 A.D. is now a dwarf nova, age-dated by its proper motion
, 2017Classical novae are stellar outbursts powered by thermonuclear runaways in the hydrogen-rich envelopes of white-dwarf stars 1,2 , accreted from close-binary red dwarf 3 or red giant 4 companions.
M. Shara +14 more
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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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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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Recent Observations of Dwarf Novae
International Astronomical Union Colloquium, 1979A supermaximum of VW Hydri was observed at the ESO site from Oct. 26 until Nov. 9» 1978. High time resolution polarimetrie and spectroscopic measurements have been obtained. This paper reports on some preliminary results.
R. Schoembs, N. Vogt
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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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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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Publications of the Astronomical Society of Australia, 1974
The object EX Hya is a dwarf nova with a binary period of 98.3 min (Mumford 1964, 1967). Warner (1972, 1973a) has observed two complete cycles of this star with a photoelectric time resolution of 5 sec. These observations suggested that EX Hya can be understood in terms of the model proposed by Warner and Nather (1971) in their discussion of U Gem.
R. D. Watson, P. T. Rayner
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The object EX Hya is a dwarf nova with a binary period of 98.3 min (Mumford 1964, 1967). Warner (1972, 1973a) has observed two complete cycles of this star with a photoelectric time resolution of 5 sec. These observations suggested that EX Hya can be understood in terms of the model proposed by Warner and Nather (1971) in their discussion of U Gem.
R. D. Watson, P. T. Rayner
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