[PDF] Top 20 The evolution of cataclysmic variables

... Given the theoretical CVs space density and assuming to detect systems out to ' 350 pc, we expect to find 0.48 CVs per square degree, that is a total of 67 CVs. Assuming that period bouncers make up for 70 per cent of ... See full document

... Cataclysmic Variables (CVs) are close binary stars in which a white dwarf is accreting material from a low-mass donor ...secular evolution of CVs. The currently ac- cepted picture of CV ... See full document

... Cataclysmic variables (CVs) are close binary stars consisting of a red-dwarf secondary transferring material on to a white-dwarf primary via an accretion disc or magnetic accretion ...origin, ... See full document

... Obtaining surface images of the secondary star in CVs has far- reaching implications. For example, a knowledge of the irradiation pattern on the inner hemisphere of the secondary star in CVs is essential if one is to ... See full document

... of cataclysmic variable (CV) evolution is the need to explain the observed lack of accreting systems in the 2–3 h orbital period range, known as the period ... See full document

... Given the ubiquity of line emission amongst CVs, emis- sion line surveys offer a powerful way to find new CVs (for a current example of such a CV search, see G¨ ansicke et al. 2002 and Aungwerojwit et al. 2005). What ... See full document

... CV evolution by draining angular momentum from the binary through a process known as magnetic braking ...CV evolution, Andronov, Pinsonneault & Sills (2003) have noted that it is unclear if magnetic ... See full document

... In agreement with previous results, most pre-CV secondary stars in our sample turned out to have spectral types > ∼ M2V, and therefore will not evolve within Hubble time (e.g. Pols et al. 1998). As discussed in Sect. ... See full document

... in cataclysmic variables (CVs) and low-mass X-ray binaries (LMXBs), using the new catalogue of Ritter & Kolb as a starting ...for evolution, with secondary stars which are slightly too large for ... See full document

... The orbital period is the most readily observable property of a CV, and provides important clues to the evolutionary state of the system. CVs evolve from long (few hours) to short periods, down to a mini- mum of ∼ 80 ... See full document

... As well as the parameters described above, the model also provides an estimate of the flux contribution from the white dwarf, bright spot, accretion disc and donor. The white dwarf temperature and distance are found by ... See full document

... e evolution of CVs and a n g u la r m om entum losses can be found in F ran k , King & R aine (1992), K ing (1988), Iben (1991) an d a recen t overview is given in W arner (1996) a n d references th erein ... See full document

... Figure 8 shows the comparable relation between orbital period and IR excess at 5.7 and 7.9 μm. V442 Oph and WX Ari are, again, outliers in the 7.9 μm data set (less so in the 5.7 μm data set). The linear fits to the ... See full document

... Obtaining surface images of CV secondaries has much wider implications, however, than just providing information on the detailed properties of these stars. For example, a knowledge of the irradiation pattern on the inner ... See full document

... Cataclysmic variables (CVs) are semidetached binary systems in which a white dwarf primary accretes material from a Roche lobe filling ...CV evolution, (see, ... See full document

... become cataclysmic variables begin as binaries separated by a few hundred solar radii, orbiting every ∼ 10 ...orbital evolution inside the envelope is then driven by dynamical friction which extracts ... See full document

... With the exception of the double-degenerate system GP Com, which will be discussed in more detail below, the spectra of the nova-like variables in Fig. 2 are dominated by strong, single- peaked emission lines of H ... See full document

... We present K-band spectra of the short-period dwarf novae YZ Cnc, LY Hya, BK Lyn, T Leo, SW UMa and WZ Sge, the nova-like variables DW UMa, V1315 Aql, RW Tri, VY Scl, UU Aqr and GP Com, and a series of field dwarf ... See full document

... While the full suite of mass-loss rates described by Hurley, Pols & Tout (2000) was used it was found that, in order to generate su ffi cient low-mass WDs, it was necessary to take η = 1.0 for Reimers’ mass-loss ... See full document

... Abstract. The flow structure in magnetic cataclysmic variables was investigated taking into account the e ff ects of strong magnetic field and fast rotation of the white dwarf. We modeled the AE Aqr system ... See full document