Hostname: page-component-848d4c4894-cjp7w Total loading time: 0 Render date: 2024-07-02T22:36:42.287Z Has data issue: false hasContentIssue false
  • English
  • Français

Are most Cataclysmic Variables in Globular Clusters dynamically formed?

Published online by Cambridge University Press:  11 March 2020

Diogo Belloni Open the ORCID record for Diogo Belloni [Opens in a new window] ,
Mirek Giersz Open the ORCID record for Mirek Giersz [Opens in a new window] ,
Liliana E. Rivera Sandoval ,
Abbas Askar Open the ORCID record for Abbas Askar [Opens in a new window]  and
Pawel Ciecielag
Diogo Belloni
Affiliation:
National Institute for Space Research, São José dos Campos, Brazil Instituto de Física y Astronomía, Universidad de Valparaíso, Valparaíso, Chile email: [email protected]
Mirek Giersz
Affiliation:
Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences, Warsaw, Poland email: [email protected]
Liliana E. Rivera Sandoval
Affiliation:
Department of Physics and Astronomy, Texas Tech University, Lubbock, USA email: [email protected]
Abbas Askar
Affiliation:
Lund Observatory, Lund University, Lund, Sweden email: [email protected]
Pawel Ciecielag
Affiliation:
Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences, Warsaw, Poland email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have been investigating populations of cataclysmic variables (CVs) in a set of more than 300 globular cluster (GC) models evolved with themoccacode.[-120pt] One of the main questions we have intended to answer is whether most CVs in GCs are dynamically formed or not. 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. In particular, we found that, on average, the detectable CV population is predominantly composed of CVs formed via a typical common envelope phase (≳70 per cent). However, core-collapsed models tend to have higher fractions of bright CVs than non-core-collapsed ones, which suggests then that the formation of CVs is indeed slightly favoured through strong dynamical interactions in core-collapsed GCs, due to the high stellar densities in their cores.

Keywords

methods: numericalnovaecataclysmic variablesglobular clusters: generalbinaries: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 404 - 407
Copyright
© International Astronomical Union 2020

References

Belczynski, K., Kalogera, V., & Bulik, T., ApJ, 572, 407CrossRefGoogle Scholar
Belloni, D., Giersz, M., Askar, A., Leigh, N., & Hypki, A., MNRAS, 462, 2950, 2016CrossRefGoogle Scholar
Belloni, D., Giersz, M., Rocha-Pinto, H. J., Leigh, N. W. C., & Askar, A., MNRAS, 464, 4077, 2017aCrossRefGoogle Scholar
Belloni, D., Zorotovic, M., Schreiber, M. R., Leigh, N. W. C., Giersz, M., & Askar, A., MNRAS, 468, 2429, 2017bCrossRefGoogle Scholar
Belloni, D., Askar, A., Giersz, M., Kroupa, P., & Rocha-Pinto, H. J., MNRAS, 471, 2812, 2017cCrossRefGoogle Scholar
Belloni, D., Kroupa, P., Rocha-Pinto, H. J., & Giersz, M., MNRAS, 474, 3740, 2018aCrossRefGoogle Scholar
Belloni, D., Schreiber, M. R., Zorotovic, M., Iłkiewicz, K., Hurley, J. R., Giersz, M., & Lagos, F., MNRAS, 478, 5639, 2018bCrossRefGoogle Scholar
Belloni, D., Giersz, M., Rivera Sandoval, L. E., Askar, A., & Ciecielag, P., MNRAS, 483, 315, 2019CrossRefGoogle Scholar
Cheng, Z., Li, Z., Xu, X., & Li, X., ApJ, 858, 33, 2018CrossRefGoogle Scholar
Cohn, H. N., et al., ApJ, 722, 20, 2010CrossRefGoogle Scholar
Cool, A. M., et al., ApJ 763, 126, 2013CrossRefGoogle Scholar
Fregeau, J. M., Cheung, P., Portegies Zwart, S. F., & Rasio, F. A., MNRAS, 352, 1, 2004CrossRefGoogle Scholar
Giersz, M., Heggie, D. C., Hurley, J. R., & Hypki, A., MNRAS, 431, 2184, 2013CrossRefGoogle Scholar
Henleywillis, S., et al., MNRAS, 479, 2834, 2018CrossRefGoogle Scholar
Hong, J., Vesperini, E., Belloni, D., & Giersz, M., MNRAS, 464, 2511, 2017CrossRefGoogle Scholar
Hypki, A. & Giersz, M., MNRAS, 429, 1221, 2013CrossRefGoogle Scholar
Hurley, J. R., Tout, C. A., & Pols, O. R., MNRAS, 329, 897, 2002CrossRefGoogle Scholar
Lugger, P. M., Cohn, H. N., Cool, A. M., Heinke, C. O., & Anderson, J., ApJ 841, 53, 2017CrossRefGoogle Scholar
Pooley, D. & Hut, P., ApJL, 646, L143, 2006CrossRefGoogle Scholar
Rivera Sandoval, L. E., et al., MNRAS, 475, 4841, 2018CrossRefGoogle Scholar
Warner, B., Cataclysmic Variable Stars, Cambridge, 1995CrossRefGoogle Scholar