On the Dark Matter’s Halo Theoretical Description


We argued that the standard field scalar potential couldn’t be widely used for getting the adequate galaxies’ curve lines and determining the profiles of dark matter their halo. For discovering the global properties of scalar fields that can describe the observable characteristics of dark matter on the cosmological space and time scales, we propose the simplest form of central symmetric potential celestial-mechanical type, i.e. U(φ) = –μ/φ. It was shown that this potential allows get rather satisfactorily dark matter profiles and rotational curves lines for dwarf galaxies. The good agreement with some previous results, based on the N-body simulation method, was pointed out. A new possibility of dwarf galaxies’ masses estimation was given, also.

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L. L. M. Chechin, "On the Dark Matter’s Halo Theoretical Description," Journal of Modern Physics, Vol. 3 No. 5, 2012, pp. 377-382. doi: 10.4236/jmp.2012.35052.

Conflicts of Interest

The authors declare no conflicts of interest.


[1] E. Komatsu, K. M. Smith, J. Dunkley, et al., “Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation,” Astrophysical Journal Supplement, Vol. 192, No. 2, 2011, Article ID 18.
[2] D. Larson, J. Dunkley, G. Hinshaw, et al., “Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Power Spectra and WMAP-Derived Parameters,” Astrophysical Journal Supplement, Vol. 192, No. 2, 2011, Article ID 16.
[3] H. Henk and J. Bhuvnesh, “Weak Gravitational Lensing and Its Cosmological Applications,” Annual Review of Nuclear and Particle Science, Vol. 58, 2008, pp. 99-123.
[4] A. F. Zakharov and M. V. Sazhin, “Gravitational Microlensing,” Physics-Uspekhi (Advanced in Physics Science), Vol. 41, No. 10, 1998, pp. 945-982.
[5] A. G. Doroshkevich, V. N. Lukash and E. V. Mikheeva, “A Solution of the Problems of Cusps and Rotation Curves in Dark Matter Halos in the Cosmological Standard Model,” Physics-Uspekhi (Advanced in Physics Science), Vol. 55, No. 1, 2012, pp. 3-18.
[6] F. Zwicky, “On the Masses of Nebulae and of Clusters of Nebulae,” Astrophysical Journal, Vol. 86, 1937, pp. 217- 246. doi:10.1086/143864
[7] D. Clowe, M. Brada?, A. H. Gonzales, et al., “A Direct Empirical Proof of the Existence of Dark Matter,” Astrophysical Journal, Vol. 648, No. 2, 2006, pp. L109-L113.
[8] G. de Luca, G. Kaufmann, V. Springel, et al., “Substructures in Dark Matter Haloes,” Monthly Notices of the Royal Astronomical Society, Vol. 348, No. 1, 2003.
[9] B. Moore, S. Ghigna, F. Governato, et al., “Dark Matter Substructure in Galactic Halo,” Astrophysical Journal Letters, Vol. 524, 1999, pp. L19-L22.
[10] D. S. Gorbunov and V. A. Rubakov, “Introduction to Theory of Early Universe,” URSS, Moscow, 2009 (in Russian).
[11] A. Susan, R. Kassin, S. de Jong and B. J. Weiner, “Dark and Baryonic Matter in Bright Spiral Galaxies: II. Radial Distributions for 34 Galaxies,” Astrophysical Journal, Vol. 643, No. 2, 2006, pp. 804-824.
[12] J. F. Navarro, C. S. Frenk and S. D. M. White, “A Universal Density Profile from Hierarchical Clustering,” Astrophysical Journal, Vol. 490, 1997, p.493.
[13] A. Burket, “The Structure of Dark Matter Haloes in Dwarf Galaxies,” Astrophysical Journal, Vol. 447, 1995, pp. L25-L28.
[14] R. Catena and P. Ullio, “A Novel Determination of the Local Dark Mater Density,” Journal of Cosmology and Astroparticle Physics, Vol. 2010, 2010.
[15] A. Loeb and N. Weiner, “Cores in Dwarf Galaxies from Dark Matter with a Yukava Potential,” Physical Review Letters, Vol. 106, No. 17, 2010, pp. 1302-1307.
[16] E. Schmutzer, “Symmetrien und Erhaltungss?tze der Physik,” Akademie Verlag, Berlin, 1972.
[17] H. Goldstein, Ch. Poole and J. Safko, “Classic Mechanics,” Addison Wesley, Reading, 2002.
[18] L. D. Landau and E. M. Lifshitz, “Mechanics,” 3rd Edition, Pergamon Press, Oxford, 1976.
[19] E. Rasia, G. Tormen and L. Moscardini, “A Dynamical Model for the Distribution of Dark Matter and Gas in Galaxy Cluster,” Monthly Notice of the Royal Astronomic Society, Vol. 351, 2004, pp. 237-252;
[20] S. Kazantzidis, L. Mayer and Ch. Mastropietro, “Density Profiles of Cold Dark Matter Substructure: Implications for the Missing-Satellites Problem,” Astrophysical Journal, Vol. 608, 2004, pp. 663-679.
[21] W. Dehnen and D. E. McLaughlin, “Dynamical Insight into Dark-Matter Haloes,” Monthly Notices of the Royal Astronomical Society, Vol. 363, 2005, pp. 1057-1068.
[22] A. Kravtsov and A. A. Klypin, “The Cores of Dark Matter Dominates Galaxies: Theory vs. Observations,” Astrophysical Journal, Vol. 502, No. 1, 1997, p. 48.
[23] I. D. Karachentsev, “Hidden Mass in the Local Group,” Physics-Uspekhi (Advanced in Physics Science), Vol. 44, No. 8, 2001, pp. 817-818. doi:10.1070/PU2001v044n08ABEH000969
[24] G. Gilmore, M. J. Wilkinson, et al., “The Observed Properties of Dark Matter on Small Spatial Scales,” Astrophysical Journal, Vol. 663, 2007, pp. 948-959.
[25] E. L. Sholnik, M. C. Liu, I. N. Reid, T. Dupuy and A. J. Weinberger, “Searching for Young Dwarfs with GALEX,” astro-ph/1011.2708v2.

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