The astrophysics of cataclysmic variables and related objects : proceedings of a meeting held in Strasbourg, France, 11-16 July 2004

By J. Hameury, Jan Lasota. 2005

363 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/95749a0e04fe7e6a3e86d871b3f5600fd610e410

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

Citations in the corpus

The 511 keV emission from positron annihilation in the Galaxy (2010, background): “The ejected mass is ∼10−4 M⊙ and is substantially enriched with the material of the white dwarf, leading to CO or to ONe novae (see, e.g. Hernanz, 2005 for a review).”
SDSS unveils a population of intrinsically faint cataclysmic variables at the minimum orbital period (2009, background): “It is therefore subject to complex selection effects (Gänsicke 2005), and should not be expected to provide a genuine representation of the intrinsic properties of the Galactic CV population.”
J-PLUS: The Javalambre Photometric Local Universe Survey (2015, background): “Historically, CVs have been discovered through their variability properties and, most recently, as by-products of quasar searches (for a review, see Gänsicke 2005).”
Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “…& Cooney 2012 Cataclysmic variables Mass transferring WD+MS stars (novae, dwarf novae, polars [AM Herculis and DQ Herculis stars], etc.) Warner 2003 AM Canis Venaticorum Helium-rich, mass transferring WD+MS stars Nelemans 2005 Algols The evolved star is less massive than the non-evolved star.”
Are the Models for Type Ia Supernova Progenitors Consistent with the Properties of Supernova Remnants? (2007, background): “Several observational and theoretical arguments point to SD-Ch explosions as the most promising route to Type Ia SNe, but there are still many uncertainties associated with this paradigm (for discussions, see Branch et al. 1995; Tout 2005).”
X-Ray Emissions from Accreting White Dwarfs: A Review (2017, background): “The emission lines in SS Cyg and U Gem are found to become broader during outburst (Mauche et al. 2005).”
Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog (2019, background): “Closely related to the CVs are the AM CVn systems, compact binaries (orbital periods 1 hr) where a WD accretes hydrogenpoor material from either an He WD or naked He star (e.g., Paczyński 1967; Marsh et al. 2004; Nelemans 2005).”
Magnetic White Dwarfs (2015, background): “…(eg Visvanathan and Wickramasinghe 1979; Wickramasinghe et al. 1989; Ferrario et al. 1994; Schwope and Beuermann 1990a; Schwope et al. 1995), and in a few systems with the highest field strengths also at ultraviolet wavelengths (eg Rosen et al. 2001; Gänsicke et al. 2001; Ferrario et al. 2003).”
Faint Thermonuclear Supernovae from AM Canum Venaticorum Binaries (2007, background): “Subject headings: binaries: close— novae, cataclysmic variables— supernovae: general— white dwarfs 1.”
AM CVn Stars: Status and Challenges (2010, background): “Two short-period CVs with evolved hydrogen-rich donors (El Psc and V485 Cen) are so far known below the nominal CV period minimum (Gänsicke 2005).”