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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

MOCCA-SURVEY database I. Accreting white dwarf binary systems in globular clusters - IV. Cataclysmic variables - properties of bright and faint populations

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Belloni, Diogo [1, 2] ; Giersz, Mirek [1] ; Sandoval, Liliana E. Rivera [3] ; Askar, Abbas [1, 4] ; Ciecielag, Pawel [1]
Total Authors: 5
[1] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw - Poland
[2] Natl Inst Space Res, Ave Astronautas 1758, BR-12227010 Sao Jose Dos Campos - Brazil
[3] Texas Tech Univ, Dept Phys & Astron, Box 41051, Sci Bldg, Lubbock, TX 79409 - USA
[4] Lund Univ, Dept Astron & Theoret Phys, Lund Observ, Box 43, SE-22100 Lund - Sweden
Total Affiliations: 4
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 483, n. 1, p. 315-331, FEB 2019.
Web of Science Citations: 4

We investigate here populations of cataclysmic variables (CVs) in a set of 288 globular cluster (GC) models evolved with the MOCCA code. This is by far the largest sample of GC models ever analysed with respect to CVs. Contrary to what has been argued for a long time, we found that dynamical destruction of primordial CV progenitors is much stronger in GCs than dynamical formation of CVs, and that dynamically formed CVs and CVs formed under no/weak influence of dynamics have similar white dwarf mass distributions. In addition, we found that, on average, the detectable CV population is predominantly composed of CVs formed via a typical common envelope phase (CEP) (greater than or similar to 70 per cent), that only approximate to 2-4 per cent of all CVs in a GC are likely to be detectable, and that core-collapsed models tend to have higher fractions of bright CVs than non-core-collapsed ones. We also consistently show, for the first time, that the properties of bright and faint CVs can be understood by means of the pre-CV and CV formation rates, their properties at their formation times and cluster half-mass relaxation times. Finally, we show that models following the initial binary population proposed by Kroupa and set with low CEP efficiency better reproduce the observed amount of CVs and CV candidates in NGC 6397, NGC 6752 and 47 Tuc. To progress with comparisons, the essential next step is to properly characterize the candidates as CVs (e.g. by obtaining orbital periods and mass ratios). (AU)

FAPESP's process: 17/14289-3 - Magnetic Cataclysmic variables: secular evolution with the BSE code and emission modelling with the CYCLOPS code
Grantee:Diogo Teixeira Belloni
Support type: Scholarships in Brazil - Post-Doctorate
FAPESP's process: 13/26258-4 - Superdense matter in the universe
Grantee:Manuel Máximo Bastos Malheiro de Oliveira
Support type: Research Projects - Thematic Grants