Abstract
The population synthesis method is used to study the possibility of explaining the appreciable fraction of the intergalactic type-Ia supernovae (SN Ia), 20 −15 +12 %, observed in galaxy clusters (Gal-Yam et al. 2003) when close white dwarf binaries merge in the cores of globular clusters. In a typical globular cluster, the number of merging double white dwarfs does not exceed ∼10−13 per year per average cluster star in the entire evolution time of the cluster, which is a factor of ∼3 higher than that in a Milky-Way-type spiral galaxy. From 5 to 30% of the merging white dwarfs are dynamically expelled from the cluster with barycenter velocities up to 150 km s−1. SN Ia explosions during the mergers of double white dwarfs in dense star clusters may account for ∼1% of the total rate of thermonuclear supernovae in the central parts of galaxy clusters if the baryon mass fraction in such star clusters is ∼0.3%.
Key words
supernovae globular clusters stellar evolutionPreview
Unable to display preview. Download preview PDF.
References
- 1.M. Bellazzinni, P. F. Fusi, P. Montegriffo, et al., Astron. J. 123, 2541 (2002).ADSGoogle Scholar
- 2.E. Capellaro, M. Turatto, D. Yu. Tsvetkov, et al., Astron. Astrophys. 322, 431 (1997).ADSGoogle Scholar
- 3.N. N. Chugai and L. R. Yungel'son, Pis'ma Astron. Zh. 30, 83 (2004); astro-ph/0308297 (2003).Google Scholar
- 4.N. V. Dunina-Barkovskaya, V. S. Imshennik, and S. I. Blinnikov, Pis'ma Astron. Zh. 27, 412 (2001) [Astron. Lett. 27, 353 (2001)].Google Scholar
- 5.M. B. Davis, W. Benz, and J. G. Hills, Astrophys. J. 424, 870 (1994).ADSGoogle Scholar
- 6.J. M. Fregeau, M. A. Gurkan, K. J. Joshi, and F. A. Rasio, Astrophys. J. (in press); astro-ph/0301521 (2003).Google Scholar
- 7.M. Hamuy, M. M. Phillips, N. B. Suntzeff, et al., Nature (in press); astro-ph/0306270 (2003).Google Scholar
- 8.W. E. Harris, Astron. J. 112, 1487 (1996).CrossRefADSGoogle Scholar
- 9.D. C. Heggie, C. Douglas, and P. Hut, Astrophys. J., Suppl. Ser. 85, 347 (1993).CrossRefADSGoogle Scholar
- 10.D. C. Heggie, P. Hut, and S. L. W. McMillan, Astrophys. J. 467, 359 (1996).CrossRefADSGoogle Scholar
- 11.M. Hilker, astro-ph/0210466 (2002).Google Scholar
- 12.F. Hoyle and W. A. Fauler, Astrophys. J. 132, 565 (1960 ).CrossRefADSGoogle Scholar
- 13.J. R. Hurley, C. A. Tout, and O. R. Pols, Mon. Not. R. Astron. Soc. 329, 897 (2002).CrossRefADSGoogle Scholar
- 14.I. Iben, Jr. and A. V. Tutukov, Astrophys. J., Suppl. Ser. 54, 355 (1984).CrossRefADSGoogle Scholar
- 15.A. Gal-Yam, D. Maoz, P. Guhathakurta, and A. V. Filippenko, Astron. J. 125, 1087 (2003).CrossRefADSGoogle Scholar
- 16.S. S. Kim and H. M. Lee, Astron. Astrophys. 347, 123 (1999).ADSGoogle Scholar
- 17.S. S. Kim, H. M. Lee, and J. Goodman, Astrophys. J. 495, 786 (1998).CrossRefADSGoogle Scholar
- 18.B. V. Kukarkin, Globular Star Clusters (Nauka, Moscow, 1974) [in Russian].Google Scholar
- 19.M. G. Lee, J. Korean Astron. Soc. 35, 1 (2002).ADSGoogle Scholar
- 20.W. Lee, A. V. Filippenko, R. R. Treffers, et al., Astrophys. J. 546, 734 (2001).ADSGoogle Scholar
- 21.V. M. Lipunov, K. A. Postnov, and M. E. Prokhorov, Astrophys. Space Sci. Rev. 9, 1 (1996).Google Scholar
- 22.M. Livio and A. Riess, submitted to the Astrophys. J.; astro-ph/0308018.Google Scholar
- 23.A. B. Marchant and S. L. Shapiro, Astrophys. J. 234, 317 (1979).CrossRefADSGoogle Scholar
- 24.R. W. Michie, Mon. Not. R. Astron. Soc. 125, 127 (1963 ).MathSciNetADSGoogle Scholar
- 25.S. Mikkola, Mon. Not. R. Astron. Soc. 208, 75 (1984).ADSGoogle Scholar
- 26.R. Napiwotzki, N. Christlieb, H. Drechsel, et al., Messenger 112, 25 (2003).ADSGoogle Scholar
- 27.G. Nelemans, L. R. Yungelson, S. F. Portegies Zwart, and F. Verbunt, Astron. Astrophys. 365, 491 (2001).CrossRefADSGoogle Scholar
- 28.K. Nomoto, Astrophys. J. 253, 798 (1982).CrossRefADSGoogle Scholar
- 29.S. Perlmutter, G. Albering, G. Goldhaber, et al., Astrophys. J. 517, 565 (1999).CrossRefADSGoogle Scholar
- 30.D. Pooley, W. H. Lewin, S. F. Anderson, et al., Astrophys. J. 591, 131 (2003).CrossRefADSGoogle Scholar
- 31.A. G. Riess, A. V. Filippenko, P. Challis, et al., Astron. J. 116, 1009 (1998).CrossRefADSGoogle Scholar
- 32.E. P. Rubinstein and C. D. Bailyn, Astrophys. J. 474, 701 (1997).ADSGoogle Scholar
- 33.S. L. Shapiro and A. B. Marchant, Astrophys. J. 225, 603 (1978).CrossRefMathSciNetADSGoogle Scholar
- 34.M. M. Shara and J. R. Hurley, Astrophys. J. 571, 830 (2002).CrossRefADSGoogle Scholar
- 35.E. I. Sorokina, S. I. Blinnikov, and O. S. Bartunov, Pis'ma Astron. Zh. 26, 90 (2000) [Astron. Lett. 26, 67 (2000)].Google Scholar
- 36.L. Spitzer, Jr., Dynamical Evolution of Globular Clusters (Princeton Univ. Press, Princeton, 1987; Mir, Moscow, 1990).Google Scholar
- 37.J. L. Tonry, B. P. Schmidt, B. Barris, et al., Astrophys. J. (in press); astroph/0305008 (2003).Google Scholar
- 38.N. Trentham and R. B. Tully, Mon. Not. R. Astron. Soc. 335, 712 (2002).CrossRefADSGoogle Scholar
- 39.S. van den Berg, Li Weidong, and A. Filippenko, Publ. Astron. Soc. Pac. (in press); astro-ph/0308195 (2003).Google Scholar
- 40.R. F. Webbink, Astrophys. J. 277, 355 (1984).CrossRefADSGoogle Scholar
- 41.J. Whelan and I. Iben, Jr., Astrophys. J. 186, 1007 (1973).CrossRefADSGoogle Scholar