How Dark Energy Affects the MOND Theory in Clusters


Modified Newtonian Dynamics (MOND) is one of the successful theories to explain the dark matter problem in galaxies. However, the data from clusters and the cosmic microwave background (CMB) indicate some dark matter should exist in larger scales. In addition, recent dynamical studies of clusters show that the effect of dark energy should not be ignored in cluster scale. In this article, I will demonstrate how dark energy affects the cluster mass calculation by using MOND. Also, I will show that the calculated cluster mass is consistent with the total matter to baryonic matter ratio obtained by the CMB data.

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Chan, M. (2012) How Dark Energy Affects the MOND Theory in Clusters. Journal of Modern Physics, 3, 1128-1130. doi: 10.4236/jmp.2012.329147.

Conflicts of Interest

The authors declare no conflicts of interest.


[1] G. Gentile, P. Salucci, U. Klein, D. Vergani and P. Kalberla, “The Cored Distribution of Dark Matter in Spiral Galaxies,” Monthly Notices of the Royal Astronomical Society, Vol. 351, No. 3, 2004, pp. 903-922. doi:10.1111/j.1365-2966.2004.07836.x
[2] G. Gilmore, M. Wilkinson, J. Kleyna, A. Koch, W. Evans, R. F. G. Wyse and E. K. Grebel, “Observed Properties of Dark Matter: Dynamical Studies of dSph Galaxies,” Nuclear Physics B: Proceedings Supplements, Vol. 173, 2007, pp. 15-18. doi:10.1016/j.nuclphysbps.2007.08.143
[3] B. Moore, S. Ghigna, F. Governato, G. Lake, T. Quinn, J. Stadel and P. Tozzi, “Dark Matter Substructure within Galactic Halos,” The Astrophysical Journal Letters, Vol. 524, No. 1 1999, p. L19. doi:10.1086/312287
[4] M. Milgrom, “MOND and the Mass Discrepancies in Tidal Dwarf Galaxies,” The Astrophysical Journal Letters, Vol. 667, No. 1, 2007, p. L45. doi:10.1086/522049
[5] M. Milgrom, “A Modification of the Newtonian Dynamics as a Possible Alternative to the Hidden Mass Hypothesis,” Astrophysical Journal, Vol. 270, 1983, pp. 365-370. doi:10.1086/161130
[6] R. H. Sanders and S. S. McGaugh, “Modified Newtonian Dynamics as an Alternative to Dark Matter,” Annual Review of Astronomy and Astrophysics, Vol. 40, 2002, pp. 263-317. doi:10.1146/annurev.astro.40.060401.093923
[7] G. W. Angus, “Is an 11 eV Sterile Neutrino Consistent with Clusters, the Cosmic Microwave Background and Modified Newtonian Dynamics?” Monthly Notices of the Royal Astronomical Society, Vol. 394, No. 1, 2009, pp. 527-532. doi:10.1111/j.1365-2966.2008.14341.x
[8] R. H. Sanders, “The Virial Discrepancy in Clusters of Galaxies in the Context of Modified Newtonian Dynamics,” The Astrophysical Journal Letters, Vol. 512, No. 1, 1999, p. L23. doi:10.1086/311865
[9] P. Natarajan and H. Zhao, “MOND Plus Classical Neutrinos Are Not Enough for Cluster Lensing,” Monthly Notices of the Royal Astronomical Society, Vol. 389, No. 1, 2008, pp. 250-256. doi:10.1111/j.1365-2966.2008.13552.x
[10] R. H. Sanders, “Neutrinos as Cluster Dark Matter,” Monthly Notices of the Royal Astronomical Society, Vol. 380, No. 1, 2007, pp. 331-338. doi:10.1111/j.1365-2966.2007.12073.x
[11] R. Takahashi and T. Chiba, “Weak Lensing of Galaxy Clusters in Modified Newtonian Dynamics,” The Astrophysical Journal, Vol. 671, No. 1, 2007, p. 45. doi:10.1086/522564
[12] G. W. Angus, B. Famaey and D. A. Buote, “X-Ray Group and Cluster Mass Profiles in MOND: Unexplained Mass on the Group Scale,” Monthly Notices of the Royal Astronomical Society, Vol. 387, No. 4, 2008, pp. 1470-1480. doi:10.1111/j.1365-2966.2008.13353.x
[13] G. W. Angus, B. Famaey and A. Diaferio, “Equilibrium Configurations of 11 eV Sterile Neutrinos in MONDian Galaxy Clusters,” Monthly Notices of the Royal Astronomical Society, Vol. 402, No. 1, 2010, pp. 395-408. doi:10.1111/j.1365-2966.2009.15895.x
[14] D. N. Spergel, et al., “Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology,” The Astrophysical Journal Supplement Series, Vol. 170, No. 2, 2007, p. 377. doi:10.1086/513700
[15] M. Maltoni and T. Schwetz, “Sterile Neutrino Oscillations after First MiniBooNE Results,” Physical Review D, Vol. 76, 2007, Article ID: 093005.
[16] M. Milgrom, “MD or DM? Modified Dynamics at Low Accelerations vs Dark Matter,” Proceedings of Science (Quarks, Strings and the Cosmos—Hector Rubinstein Memorial Symposium), Stockholm, 9-11 August 2010.
[17] A. Chernin, P. Teerikorpi and Y. Baryshev, “Why Is the Hubble Flow So Quiet?” Advances in Space Research, Vol. 31, No. 2, 2003, pp. 459-467. doi:10.1016/S0273-1177(02)00731-7
[18] G. S. Bisnovatyi-Kogan and A. D. Chernin, “Dark Energy and Key Physical Parameters of Clusters of Galaxies,” Astrophysics and Space Science, Vol. 338, 2012, p. 337.
[19] I. King, “Density Data and Emission Measure for a Model of the Coma Cluster,” The Astrophysical Journal, Vol. 174, 1972, p. L123. doi:10.1086/180963
[20] J. J. Mohr, B. Mathiesen and A. E. Evrard, “Properties of the Intracluster Medium in an Ensemble of Nearby Gal- axy Clusters,” The Astrophysical Journal, Vol. 517, No. 2, 1999, p. 627. doi:10.1086/307227
[21] A. A. Aguilar-Arevalo, et al., “Search for Electron Neutrino Appearance at the s△m2~1 eV2 Scale,” Physical Review Letters, Vol. 98, 2007, Article ID: 231801.

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