Holographic Principle and Large Scale Structure in the Universe
T. R. Mongan
DOI: 10.4236/jmp.2011.212187   PDF    HTML   XML   4,437 Downloads   7,866 Views   Citations


A reasonable representation of large scale structure, in a closed universe so large it’s nearly flat, can be developed by extending the holographic principle and assuming the bits of information describing the distribution of matter density in the universe remain in thermal equilibrium with the cosmic microwave background radiation. The analysis identifies three levels of self-similar large scale structure, corresponding to superclusters, galaxies, and star clusters, between today’s observable universe and stellar systems. The self-similarity arises because, according to the virial theorem, the average gravitational potential energy per unit volume in each structural level is the same and depends only on the gravitational constant. The analysis indicates stellar systems first formed at z ≈ 62, consistent with the findings of Naoz et al., and self-similar large scale structures began to appear at redshift z ≈ 4. It outlines general features of development of self-similar large scale structures at redshift z < 4. The analysis is consistent with observations for angular momentum of large scale structures as a function of mass, and average speed of substructures within large scale structures. The analysis also indicates relaxation times for star clusters are generally less than the age of the universe and relaxation times for more massive structures are greater than the age of the universe.

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T. Mongan, "Holographic Principle and Large Scale Structure in the Universe," Journal of Modern Physics, Vol. 2 No. 12, 2011, pp. 1544-1549. doi: 10.4236/jmp.2011.212187.

Conflicts of Interest

The authors declare no conflicts of interest.


[1] V. Bromm, et al, “Formation of the First Stars and Gal- axies,” Nature, Vol. 459, 2009, pp. 49-54.
[2] S. Battacharya, et al., “Mass Function Predictions Be- yond LCDM,” Bulletin of the American Astronomical Society, Vol. 43, 2011.
[3] R. Bousso, “The Holographic Principle,” Reviews of Modern Physics, Vol. 74, 2002, pp. 825-874.
[4] A. Siemiginowska, et al, “The 300 kpc Long X-Ray Jet in PKS 1127-145, z = 1.18 Quasar: Constraining X-Ray Emission Models,” The Astrophysical Journal, Vol. 657, 2007, p. 145. doi:10.1086/510898
[5] W. Percival, et al, “Measuring the Matter Density Using Baryon Oscillations in the SDSS,” The Astrophysical Journal, Vol. 657, No. 1, 2007, p. 51. doi:10.1086/510772
[6] C. Misner, K. Thorne and J. Wheeler, “Gravitation,” W. H. Freeman and Company, New York, 1973.
[7] S. Longair, “Galaxy Formation,” Springer-Verlag, Berlin, 1998.
[8] L. Lubin, et al, “A Definitive Optical Detection of a Supercluster at z ≈ 0.91,” The Astrophysical Journal, Vol. 531, No. 1, 2000, p. L5. doi:10.1086/312518
[9] J. de Carvalho and P. Macedo, “The Structure Formation in a Quasi-Static Approximation,” Dark and Visible Mat- ter in Galaxies. ASP Conference Series, Vol. 117, 1997, p. 310.
[10] O. Gnedin and J. Ostriker, “Destruction of the Galactic Globular Cluster System,” The Astrophysical Journal, Vol. 474, No. 1, 1997, p. 223. doi:10.1086/303441
[11] P. Crowther, “The R136 Star Cluster Hosts Several Stars Whose Individual Masses Greatly Exceed the Accepted 150 Msun Stellar Mass Limit,” Monthly Notices of the Royal Astronomical Society, Vol. 408, No. 2, pp. 731- 751.
[12] S. Naoz, et al., “The First Stars in the Universe,” MNRAS Letter, Vol. 373, No. L98, 2006.
[13] P. Massey and R. Meyer, “Stellar Masses,” pg. 1, Encyclopedia of Astronomy and Astrophysics, 2001
[14] M. Markevitch, et al., “Direct Constraints on the Dark Matter Self-Interaction Cross-Section from the Merging Galaxy Cluster 1E0657-56,” The Astrophysical Journal, Vol. 606, No. 2, 2004, p. 819. doi:10.1086/383178
[15] P. Wesson, “Clue to the Unification of Gravitation and Particle Physics,” Physical Review D, Vol. 23, No. 8, 1981, pp. 1730-1734. doi:10.1103/PhysRevD.23.1730
[16] D. Forbes and P. Kroupa, “What Is a Galaxy? Cast your vote here...,” Publications of the Astronomical Society of Australia, Vol. 28, No. 1, pp. 77-82.
[17] F. Shu, “The Physical Universe—An Introduction to Astronomy,” University Science Books, Herndon, 1982
[18] J. Binney and S. Tremaine, “Galactic Dynamics,” Princeton University Press, Princeton, 1987
[19] D. Bhattacharya, “Stellar Systems: Two-Body Relaxation,” PH217: Aug-Dec 2003, http://meghnad.iucaa.ernet.in/dipankar/ph217/relax.pdf

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