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@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 = "05 dez. 2020"
}


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