Mechanical properties of the thermal equilibrium Friedmann-Robertson-Walker universe model

doi:10.1088/1674-1056/23/5/050401

Abstract The mechanical property of the thermal-equilibrium Friedmann-Robertson-Walker (TEFRW) universe is first studied. The equation of state and the scale factor of the TEFRW universe take the forms of w=w(a;z_T) and a=a(a;z_T,H₀). For the universe consisting of the nonrelativistic matter and the dark energy, the behavior of the dark energy depends on the value of the present-day matter fraction. For the TEFRW universe consisting of N ingredients, the effective temperature is introduced. Lastly, a simple TEFRW universe model is analyzed.

Keywords: TEFRW universe dark energy effective temperature

Received: 20 August 2013
Revised: 10 October 2013
Accepted manuscript online:

PACS:	04.70.Dy	(Quantum aspects of black holes, evaporation, thermodynamics)
	04.62.+v	(Quantum fields in curved spacetime)

Fund: Project supported by the National Natural Science Foundation of China and the Liaoning Education Committee of China (Grant No. 2009A036).

Corresponding Authors: Wei Yi-Huan
E-mail: weiyihuan@263.net

About author: 04.70.Dy; 04.62.+v

Cite this article:

Wei Yi-Huan (魏益焕), Lan Tian-Bao (兰天葆), Zhang Yue-Zhu (张月竹), Fu Yan-Yan (付妍妍) Mechanical properties of the thermal equilibrium Friedmann-Robertson-Walker universe model 2014 Chin. Phys. B 23 050401

[1]	Riess A G, Filippenko A V and Challis P 1998 Astron. J. 116 1009
[2]	Perlmutter S, Aldering G and Goldhaber G 1999 Astrophys. J. 517 565
[3]	Riess A G, Strolger L G and Tonry J 2004 Astrophys. J. 607 665
[4]	Cunha J V 2009 Phys. Rev. D 79 047301
[5]	Cunha J V and Lima J A S 2008 Mon. Not. Roy. Astron. Soc. 390 210
[6]	Davis T M, Mörtsell E and Sollerman J 2007 Astrophys. J. 666 716
[7]	Astier P, Guy J and Regnault N 2006 Astron. Astrophys. 447 31
[8]	Gardner C L 2005 Nucl. Phys. B 707 278
[9]	Qiang Y and Zhang T J 2006 Mod. Phys. Lett. A 21 75
[10]	Ishida E E O, Reis R R R, Toribio A V and Waga I 2008 Astropart. Phys. 28 547
[11]	Bousso R 2005 Phys. Rev. D 71 064024
[12]	Wang B, Gong Y G and Abdalla E 2006 Phys. Rev. D 74 083520
[13]	Bernabei R, Belli P and Cappella F 2008 Euro. Phys. J. C 56 333
[14]	Aalseth C E, Barbeau P S and Bowden N S 2011 Phys. Rev. Lett. 106 131301
[15]	Aprile E, Arisaka K and Arneodo F 2011 Phys. Rev. Lett. 107 131302
[16]	Gong Y, Wang B and Wang A 2007 J. Cosmol. Astropart. Phys. 0701 024
[17]	Feng L and Lu T 2011 J. Cosmol. Astropart. Phys. 11 034
[18]	Komatsu E, Dunkley J and Nolta M R 2009 Astrophys. J. Suppl. 180 330
[19]	Alam U, Sahni V and Starobinsky A A 2004 J. Cosmol. Astropart. Phys. 0406 008
[20]	Wu P U and Yu H W 2006 Phys. Lett. B 643 315
[21]	Caldwell R R 2002 Phys. Lett. B 545 23
[22]	Wang W F, Shui Z W and Tang B 2010 Chin. Phys. B 19 119801
[23]	Lü J B, Xu L X, Liu M L and Gui Y X 2009 Chin. Phys. B 18 1711
[24]	Lima J A S and Pereira S H 2008 Phys. Rev. D 78 083504
[25]	Lima J A S and Alcaniz J S 2004 Phys. Lett. B 600 191
[26]	Banks T, Fischler W and Mannelli L 2005 Phys. Rev. D 71 123514

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Mechanical properties of the thermal equilibrium Friedmann-Robertson-Walker universe model

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