@Article{BelloniGieSanAskCie:2019:CaVaPr,
author = "Belloni, Diogo Teixeira and Giersz, Mirek and Sandoval, Liliana E.
Rivera and Askar, Abbas and Ciecielag, Pawel",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Polish
Academy of Sciences} and {Texas Tech University} and {Polish
Academy of Sciences} and {Polish Academy of Sciences}",
title = "MOCCA-SURVEY database I. accreting white dwarf binary systems in
globular clusters - IV. cataclysmic variables - properties of
bright and faint populations",
journal = "Monthly Notices of the Royal Astronomical Society",
year = "2019",
volume = "483",
number = "1",
pages = "315--331",
month = "Feb.",
keywords = "methods: numerical, novae, cataclysmic variables, globular
clusters: general, binaries: general.",
abstract = "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).",
doi = "10.1093/mnras/sty3097",
url = "http://dx.doi.org/10.1093/mnras/sty3097",
issn = "0035-8711 and 1365-2966",
language = "en",
targetfile = "belloni_mocca.pdf",
urlaccessdate = "27 abr. 2024"
}