AM CVn Stars: Status and Challenges
By J. Solheim. 2010
156 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/c8c070811b53638fd666a7856f9357a0b9ca10e0
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In Astronomy and Astrophysics
Citations in the corpus
- Models of low-mass helium white dwarfs including gravitational settling, thermal and chemical diffusion, and rotational mixing (2016, background): “Ia and Ca-rich supernovae (Bildsten et al. 2007; Iben & Tutukov 1984; Perets et al. 2010; Foley 2015), as well as exotic systems such as AM CVn stars, R Coronae Borealis (R CrB), and single subdwarf B/O stars (Kilic et al. 2014; Solheim 2010; Clayton 2013; Heber 2016).”
- Survey of period variations of superhumps in SU UMa-type dwarf novae. X. The tenth year (2017) (2009, background): “…this object is hydrogen-rich or not, we suspect that this object is a binary containing hydrogen in the secondary with an evolved core rather than a hydrogendepleted AM CVn-type binary, since the known AM CVntype objects with this Porb do not show outbursts (cf. Solheim 2010; Ramsay et al. 2012).”
- Prospects for detection of detached double white dwarf binaries with Gaia, LSST and LISA (2017, background): “…distance indicators (e.g. Riess et al. 1998; Perlmutter et al. 1999), AM CVn systems (Nelemans et al. 2001a; Marsh, Nelemans & Steeghs 2004; Solheim 2010) and ‘fast optical transients’ including Ia supernovae, Ca-rich transients and fast/bright transients (Bildsten et al. 2007; Perets et…”
- LISA verification binaries with updated distances from Gaia Data Release 2 (2018, background): “These include detached (Brown et al. 2016b) and semi-detached double white dwarfs (the latter called AM CVn type binaries; Solheim 2010), and semi-detached white dwarf-neutron star binaries (so-called ultracompact X-ray binaries; Nelemans & Jonker 2010) and double neutron stars (Lyne et al. 2004).”
- Observational Clues to the Progenitors of Type Ia Supernovae (2013, background): “…same could be true for some fraction of the so-called AM CVn systems, a class of objects in which a WD accretes helium from a very low-mass companion (see Solheim 2010 for a review), although the majority of the observed systems have evolved to too-low mass transfer rates for a double detonation.”
- X-Ray Emissions from Accreting White Dwarfs: A Review (2017, background): “Those with hydrogen-deficient donors are called the AM CVn stars (Solheim 2010): they are sometimes treated as a subclass of CVs, and sometimes considered a parallel class.”