Gravitational stability of dark energy in galaxies and clusters of galaxies

1Novosyadlyi, B, 1Tsizh, M, 1Kulinich, Y
1Astronomical Observatory of Ivan Franko National University of Lviv, Lviv, Ukraine
Kinemat. fiz. nebesnyh tel (Online) 2014, 30(2):3-15
Start Page: Problems of Astronomy
Language: Ukrainian

We analyzed the behaviour of the scalar field as dark energy of the Universe in a static world of galaxies and clusters of galaxies. We find the analytical solutions of evolution equations for the density and velocity perturbations and of dark matter and dark energy, which interact only gravitationally, along with the metric perturbations in the static world with the background Minkowski metric. Usin them it was shown that the quintessential and phantom dark energy in the static world of galaxies and clusters of galaxies is gravitationally stable and can only oscillate by the influence of self-gravity. In the gravitational field of the dark matter perturbations it is able to condense monotonically, but the amplitudeson all scales remain small. It was illustrated also, that the “accretion” of phantom dark energy in the region of dark matter overdensities causes formation of dark energy underdensities — the regions with negative amplitude of density perturbations of dark energy.

Keywords: dark energy, gravitational fields

1.L. R. Abramo, R. C. Batista, L. Liberato, and R. Rosenfeld, “Structure formation in the presence of dark energy perturbations,” J. Cosmol. Astropart. Phys. 11, id. 012(21) (2007).

2.L. Amendola and S. Tsujikawa, Dark Energy: Theory and Observations (Cambridge University Press, 2010).

3.E. Babichev, S. Chernov, V. Dokuchaev, and Y. Eroshenko, “Ultrahard fluid and scalar field in the Kerr-Newman metric,” Phys. Rev. D 78, 104027 (2008).

4.E. Babichev, S. Chernov, V. Dokuchaev, and Y. Eroshenko, “Perfect fluid and scalar field in the Reissner-Nordstrm metric,” J. Exp. Theor. Phys. 112, 784 (2011).

5.E. O. Babichev, V. I. Dokuchaev, and Y. N. Eroshenko, “Black hole mass decreasing due to phantom energy accretion,” Phys. Rev. Lett. 93, 021102 (2004).

6.E. Babichev, V. Dokuchaev, and Y. Eroshenko, “The accretion of dark energy onto a black hole,” J. Exp. Theor. Phys. 100, 528 (2005).

7.E. Babichev, V. Dokuchaev, and Y. Eroshenko, “Backreaction of accreting matter onto a black hole in the Eddington-Finkelstein coordinates,” Clas. Quant. Grav. 29, 115002 (2012).

8.J. M. Bardeen, “Gauge-invariant cosmological perturbations,” Phys. Rev. D 22, 1882–1905 (1980).

9.T. Basse, O. Eggers Bjaelde, and Y. Y. Y. Wong, “Spherical collapse of dark energy with an arbitrary sound speed,” J. Cosmol. Astropart. Phys. 10, id. 038(24) (2011).

10. Dark Energy: Observational and Theoretical Approaches, Ed. by P. Ruiz-Lapuente (Cambridge University Press, 2010).

11.S. Dutta and I. Maor, “Voids of dark energy,” Phys. Rev. D 75, id. 063507(9) (2007).

12.J. H. Jeans, “The stability of a spherical nebula,” Philosophical Transactions of the Royal Society of London. Series A 199, 1–53 (1902).

13.Yu. Kulinich, “Evolution of a spherically symmetric dust-like cloud in ACDM models,” Kinematics Phys. Celestial Bodies 24, 121–136 (2008).

14.Yu. Kulinich, B. Novosyadlyj, and S. Apunevych, “Non-linear power spectra of dark and luminous matter in halo model of structure formation,” Phys. Rev. D 88, 103505 (2013).

15.“Lectures on cosmology: Accelerated expansion of the nivese,” Lect. Notes in Physics 800, Ed. by G. Wolschin (Springer, Berlin-Heidelberg, 2010).

16.D. Mota, D. J. Shaw, and J. Silk, “On the magnitude of dark energy voids and overdensities,” Astroph. J. 675, 29–48 (2008).

17.B. Novosyadlyj, “Large-scale structure of the Universe formation: theory and observations,” Journal of Physical Studies 11, 226–257 (2007).

18.B. Novosyadlyj, V. Pelykh, Yu. Shtanov, and A. Zhuk, Dark Energy: Observational Evidence and Theoretical Models, Ed. by V. Shulga (Akademperiodyka, K., 2013).

19.B. Novosyadlyj, O. Sergijenko, S. Apunevych, and V. Pelykh, “Properties and uncertainties of scalar field models of dark energy with barotropic equation of state,” Phys. Rev. D 82, id. 103008(16) (2010).

20.B. Novosyadlyj, O. Sergijenko, R. Durrer, and V. Pelykh, “Do the cosmological observational data prefer phantom dark energy?,” Phys. Rev. D 86, id. 083008(13) (2012).

21.N. P. Pitjev and E. V. Pitjeva, “Constraints on dark matter in the solar system,” Pis’ma v Astronomicheskii Zhurnal 39, 163–172 (2013).

22.W. H. Press and P. Schechter, “Formation of galaxies and clusters of galaxies by self-similar gravitational condensation,” Astroph. J. 187, 425–438 (1974).

23.O. Sergijenko, R. Durrer, and B. Novosyadlyj, “Observational constraints on scalar field models of dark energy with barotropic equation of state,” J. Cosmol. Astropart. Phys. 08, id. 004(25) (2011).

24.O. Sergijenko, Yu. Kulinich, B. Novosyadlyj, and V. Pelykh, “Large-scale structure formation in cosmology with classical and tachyonic scalar fields,” 25, 26–39 (2009).

25.O. Sergijenko and B. Novosyadlyj, “Perturbed dark energy: Classical scalar field versus tachyon,” Phys. Rev. D 80, id. 083007(13) (2009).

26.R. Smith, J. Peacock, A. Jenkis, S. D. White, C. S. Frenk, et al., “Stable clustering, the halo model and nonlinear cosmological power spectrum,” Mon. Not. Roy. Astron. Soc. 341, 1311–1332 (2003).

27.Q. Wang and Z. Fan, “Dynamical evolution of quintessence dark energy in collapsing dark matter halos,” Phys. Rev. D 79, 123012 (2009).

28.Q. Wang and Z. Fan, “Simulation studies of dark energy clustering induced by the formation of dark matter halos,” Phys. Rev. D 85, 023002 (2012).