Abstract
An analytical model is considered for describing the inner regions of dark matter halos. This model is based on the assumption that the density of dark matter varies according to the power law. The model concerns the distribution function in phase space that is expressed in terms of the adiabatic invariants (radial action and angular momentum). Two types, narrow and broad, are suggested for the angular part of the distribution function. The model makes it possible to explicitly describe the adiabatic compression of halos due to a change induced in the gravitational potential by the condensation of baryonic matter at the center. The change in the density of the dark matter halos is calculated and it is shown that the standard algorithm for calculating the adiabatic compression overestimates the halo density, particularly for the case of strong radial anisotropy.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
G. Bertone and D. Merritt, Mod. Phys. Lett. A 20, 1021 (2005).
J. Navarro, E. Hayashi, C. Power, et al., Mon. Not. R. Astron. Soc. 349, 1039 (2004).
J. Diemand, M. Zemp, B. Moore, et al., Mon. Not. R. Astron. Soc. 364, 665 (2005).
Y. Lu, H. Mo, N. Katz, and M. Weinberg, Mon. Not. R. Astron. Soc. (in press), astro-ph/0508624.
W. Dehnen and D. McLaughlin, Mon. Not. R. Astron. Soc. 363, 1057 (2005).
C. Austin, L. Williams, E. Barnes, et al., Astrophys. J. 634, 756 (2005).
J. Taylor and J. Navarro, Astrophys. J. 563, 483 (2001).
S. Hansen and B. Moore, New Astron. 11, 333 (2006).
H. Zhao, Mon. Not. R. Astron. Soc. 278, 488 (1996).
S. Hansen, D. Egli, L. Hollenstein, and C. Salzmann, New Astron. 10, 379 (2005).
G. Mamon and E. Lokas, Mon. Not. R. Astron. Soc. 363, 705 (2005).
J. Binney and S. Tremaine, Galactic Dynamics (Princeton Univ. Press, Princeton, 1987).
P. Gondolo and J. Silk, Phys. Rev. Lett. 83, 1719 (1999).
A. V. Gurevich and K. P. Zybin, Usp. Fiz. Nauk 165, 723 (1995) [Phys. Usp. 38, 687 (1995)].
J. An and N. Evans, Astrophys. J. 642, 752 (2006).
W. Dehnen, Mon. Not. R. Astron. Soc. 360, 869 (2005).
S. Kazantzidis, A. Zentner, and A. Kravtsov, Astrophys. J. 641, 647 (2006); astro-ph/0510583.
S. Hansen, Mon. Not. R. Astron. Soc. 352, L41 (2004).
G. Blumenthal, S. Faber, R. Flores, and J. Primack, Astrophys. J. 301, 27 (1986).
O. Gnedin, A. Kravtsov, A. Klypin, and D. Nagai, Astrophys. J. 616, 16 (2004).
J. Sellwood and S. McGaugh, Astrophys. J. 634, 70 (2005).
J. Choi, Y. Lu, H. Mo, and M. Weinberg, astro-ph/0604587.
V. Cardone and M. Sereno, Astron. Astrophys. 438, 545 (2005).
G. Bertone and D. Merritt, Phys. Rev. D 72, 103502 (2005).
M. I. Zel’nikov and E. A. Vasil’ev, Pis’ma Zh. Éksp. Teor. Fiz. 81, 115 (2005) [JETP Lett. 81, 85 (2005)].
Author information
Authors and Affiliations
Additional information
Original Russian Text © E.A. Vasil’ev, 2006, published in Pis’ma v Zhurnal Éksperimental’noĭ i Teoreticheskoĭ Fiziki, 2006, Vol. 84, No. 2, pp. 49–53.