Results 31 to 40 of about 2,620,915 (156)

Pole-On Cataclysmic Variables as Be Stars [PDF]

open access: yesInternational Astronomical Union Colloquium, 1987
Cataclysmic-variable stars (CVs) are technically Be stars, since Balmer emission lines appear in their spectra. In general, CV spectra are so unusual that they are easily recognized. The main features are extremely broad, shallow hydrogen lines with broad, faint emission cores.
openaire   +1 more source

The helium-rich cataclysmic variable SBSS 1108+574 [PDF]

open access: yes, 2013
We present time-resolved spectroscopy and photometry of the dwarf nova SBSS 1108+574, obtained during the 2012 outburst. Its quiescent spectrum is unusually rich in helium, showing broad, double-peaked emission lines from the accretion disc. We measure a
Koff, R.A.   +36 more
core   +1 more source

HS 2331+3905 : the cataclysmic variable that has it all [PDF]

open access: yes, 2005
We report detailed follow-up observations of the cataclysmic variable HS 2331+3905, identified as an emissionline object in the Hamburg Quasar Survey. An orbital period of 81.08 min is unambiguously determined from the detection of eclipses in the light ...
Araujo-Betancor, S.   +21 more
core   +1 more source

Exploring the application of new telescope technologies in the testing of dwarf novae accretion models [PDF]

open access: yes, 2011
Includes abstract.Includes bibliographical references (p. 261-273.)In this thesis I investigate emerging telescope technologies and demonstrate, within the context of accretion in cataclysmic variables (CVs), their role in contributing to the stellar ...
Spark, Mellony
core   +1 more source

Spectroscopy of Nine Cataclysmic Variable Stars [PDF]

open access: yesPublications of the Astronomical Society of the Pacific, 2007
31 pages, 5 postscript and one PNG figure.
Sheets, H. A.   +4 more
openaire   +2 more sources

White Dwarfs in Cataclysmic Variable Stars: Surface Temperatures and Evolution [PDF]

open access: yesJournal of Astronomy and Space Sciences, 2012
A summary is presented of what is currently known about the surface temperatures of accreting white dwarfs (WDs) detected in non-magnetic and magnetic cataclysmic variables (CVs) based upon synthetic spectral analyses of far ultraviolet data.
Edward M. Sion
doaj   +1 more source

Newly discovered cataclysmic variables from the INT/WFC photometric Hα survey of the northern Galactic plane [PDF]

open access: yes, 2007
We report the discovery of 11 new cataclysmic variable (CV) candidates by the Isaac Newton Telescope (INT) Photometric H alpha Survey of the northern Galactic plane (IPHAS).
Roelofs, Gijs H. A.   +19 more
core   +1 more source

Accretion Discs in Cataclysmic Variable Stars [PDF]

open access: yesInternational Astronomical Union Colloquium, 1997
AbstractAn overview is given of the spatial and time-dependent properties of the accretion discs in cataclysmic variable stars.
openaire   +1 more source

In Situ Construction of Phosphorus‐Containing Crosslinked Urethane Network Combined With Ammonium Polyphosphate via Reactive Blending for Enhancing Flame Retardancy and Anti‐Dripping Performance of Polylactic Acid Composites

open access: yesSafety Science and Technology, EarlyView.
By in situ reaction blending, DOPO‐HQ and THEIC were added to PLA with MDI to construct a phosphorus containing polyurethane network, which significantly improved the flame retardant and anti‐dripping properties of polylactic acid composites. ABSTRACT Polylactic acid (PLA) is highly flammable and prone to severe melt dripping during combustion, which ...
Chiyuan Chen   +4 more
wiley   +1 more source

The S-PLUS 12-band Photometry as a Powerful Tool for Discovery and Classification: Ten Cataclysmic Variables in a Proof-of-concept Study

open access: yesThe Astrophysical Journal Letters
Multiband photometric surveys provide a straightforward way to discover and classify astrophysical objects systematically, enabling the study of a large number of targets at relatively low cost.
Raimundo Lopes de Oliveira   +11 more
doaj   +1 more source

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