New initial condition of the new agegraphic dark energy model

doi:10.1088/1674-1056/22/3/039501

中国物理B ›› 2013, Vol. 22 ›› Issue (3): 39501-039501.doi: 10.1088/1674-1056/22/3/039501

• GEOPHYSICS, ASTRONOMY, AND ASTROPHYSICS • 上一篇下一篇

New initial condition of the new agegraphic dark energy model

李云鹤, 张敬飞, 张鑫

Department of Physics, College of Sciences, Northeastern University, Shenyang 110004, China

收稿日期:2012-08-03 修回日期:2012-09-04 出版日期:2013-02-01 发布日期:2013-02-01
基金资助:
Project supported by the National Natural Science Foundation of China (Grant Nos. 10705041, 10975032, 11047112, and 11175042), the Program for New Century Excellent Talents in University of Ministry of Education of China (Grant No. NCET-09-0276), and the National Ministry of Education of China (Grant Nos. N100505001 and N110405011).

New initial condition of the new agegraphic dark energy model

Li Yun-He (李云鹤), Zhang Jing-Fei (张敬飞), Zhang Xin (张鑫)

Department of Physics, College of Sciences, Northeastern University, Shenyang 110004, China

Received:2012-08-03 Revised:2012-09-04 Online:2013-02-01 Published:2013-02-01
Contact: Zhang Xin E-mail:zhangxin@mail.neu.edu.cn
Supported by:
Project supported by the National Natural Science Foundation of China (Grant Nos. 10705041, 10975032, 11047112, and 11175042), the Program for New Century Excellent Talents in University of Ministry of Education of China (Grant No. NCET-09-0276), and the National Ministry of Education of China (Grant Nos. N100505001 and N110405011).

摘要/Abstract

摘要： The initial condition Ω_de(z_ini)=n²(1+z_ini)^-2/4 at z_ini=2000 widely used to solve the differential equation of the density of the new agegraphic dark energy (NADE) Ω_de, makes the NADE model be a single-parameter dark-energy cosmological model. However, we find that this initial condition is only applicable in a flat universe with only dark energy and pressureless matter. In fact, in order to obtain more information from current observational data, such as the cosmic microwave background (CMB) and the baryon acoustic oscillations (BAO), we need to consider the contribution of radiation. For this situation, the initial condition mentioned above becomes invalid. To overcome this shortage, we investigate the evolutions of dark energy in the matter-dominated and the radiation-dominated epochs, and obtain a new initial condition Ω_de(z_ini)=n²(1+z_ini)^-2(1+√F(z_ini)²/4 at z_ini=2000, where F(z)≡Ω_r0(1+z)/[Ω_m0+Ω_r0(1+z)] with Ω_r0 and Ω_m0 being the current density parameters of radiation and pressureless matter, respectively. This revised initial condition is applicable for the differential equation of Ω_de obtained in the standard Friedmann-Robertson-Walker (FRW) universe with dark energy, pressureless matter, radiation, and even spatial curvature, and can still keep the NADE model being a single-parameter model. With the revised initial condition and the observational data of type Ia supernova (SNIa), CMB, and BAO, we finally constrain the NADE model. The results show that the single free parameter n of the NADE model can be constrained tightly.

关键词: new agegraphic dark energy model, initial condition, single-parameter model, observational constraints

Abstract: The initial condition Ω_de(z_ini)=n²(1+z_ini)^–2/4 at z_ini=2000 widely used to solve the differential equation of the density of the new agegraphic dark energy (NADE) Ω_de, makes the NADE model be a single-parameter dark-energy cosmological model. However, we find that this initial condition is only applicable in a flat universe with only dark energy and pressureless matter. In fact, in order to obtain more information from current observational data, such as the cosmic microwave background (CMB) and the baryon acoustic oscillations (BAO), we need to consider the contribution of radiation. For this situation, the initial condition mentioned above becomes invalid. To overcome this shortage, we investigate the evolutions of dark energy in the matter-dominated and the radiation-dominated epochs, and obtain a new initial condition Ω_de(z_ini)=n²(1+z_ini)^–2(1+√F(z_ini)²/4 at z_ini=2000, where F(z)≡Ω_r0(1+z)/[Ω_m0+Ω_r0(1+z)] with Ω_r0 and Ω_m0 being the current density parameters of radiation and pressureless matter, respectively. This revised initial condition is applicable for the differential equation of Ω_de obtained in the standard Friedmann–Robertson–Walker (FRW) universe with dark energy, pressureless matter, radiation, and even spatial curvature, and can still keep the NADE model being a single-parameter model. With the revised initial condition and the observational data of type Ia supernova (SNIa), CMB, and BAO, we finally constrain the NADE model. The results show that the single free parameter n of the NADE model can be constrained tightly.

Key words: new agegraphic dark energy model, initial condition, single-parameter model, observational constraints

中图分类号: (Dark energy)

95.36.+x

98.80.Es (Observational cosmology (including Hubble constant, distance scale, cosmological constant, early Universe, etc)) 98.80.-k (Cosmology)

李云鹤, 张敬飞, 张鑫. New initial condition of the new agegraphic dark energy model[J]. 中国物理B, 2013, 22(3): 39501-039501.

Li Yun-He (李云鹤), Zhang Jing-Fei (张敬飞), Zhang Xin (张鑫). New initial condition of the new agegraphic dark energy model[J]. Chin. Phys. B, 2013, 22(3): 39501-039501.

参考文献 36

[1]	Riess A G, Filippenko A V, Challis P, Clocchiatti A, Diercks A, Garnavich P M, Gilliland R L, Hogan C J, Jha S, Kirshner R P, Leibundgut B, Phillips M M, Reiss D, Schmidt B P, Schommer R A, Smith R C, Spyromilio J, Stubbs C, Suntzeff N B and Tonry J 1998 Astron. J. 116 1009
[2]	Perlmutter S, Aldering G, GoldhaberG, et al. 1999 Astrophys. J. 517 565
[3]	Peebles P J E and Ratra B 2003 Rev. Mod. Phys. 75 559
[4]	Carroll S M 2001 Living Rev. Rel. 4 1
[5]	Lee T D 2004 Chin. Phys. Lett. 21 1187
[6]	Dvali G R, Gabadadze G and Porrati M 2000 Phys. Lett. B 485 208
[7]	Deffayet C, Dvali G R and Gabadadze G 2002 Phys. Rev. D 65 044023
[8]	Wei H and Cai R G 2008 Phys. Lett. B 660 113
[9]	Wei H and Cai R G 2008 Phys. Lett. B 663 1
[10]	Kácutearolyhácuteazy F 1966 Nuovo Cim A 42 390
[11]	Kácutearolyhácuteazy F, Frenkel A and Lukácuteacs B 1982 Physics as Natural Philosophy (Cambridge: MIT Press)
[12]	Kácutearolyhácuteazy F, Frenkel A and Lukácuteacs B 1986 Quantum Concepts in Space and Time (Oxford: Clarendon Press)
[13]	Wei H 2009 Eur. Phys. J. C 60 449
[14]	Wei H 2010 J. Cosmol. Astropart. Phys. 1008 020
[15]	Wei H 2011 J. Cosmol. Astropart. Phys. 1104 022
[16]	Zhang J F, Zhang X and Liu H Y 2008 Eur. Phys. J. C 54 303
[17]	Li M, Li X D, Wang S and Zhang X 2009 J. Cosmol. Astropart. Phys. 0906 036
[18]	Liu X L and Zhang X 2009 Commun. Theor. Phys. 52 761
[19]	Cui J L, Zhang L, Zhang J F and Zhang X 2010 Chin. Phys. B 19 019802
[20]	Li M, Li X D and Zhang X 2010 Sci. China Phys. Mech. Astron. 53 1631
[21]	Zhang L, Cui J L, Zhang J F and Zhang X 2010 Int. J. Mod. Phys. D 19 21
[22]	Liu X L, Zhang J F and Zhang X 2010 Phys. Lett. B 689 139
[23]	Zhang J F, Zhang L and Zhang X 2010 Phys. Lett. B 691 11
[24]	Li Y H, Ma J Z, Cui J L, Wang Z and Zhang X 2011 Sci. China Phys. Mech. Astron. 54 1367
[25]	Bond J R, Efstathiou G and Tegmark M 1997 Mon. Not. Roy. Astron. Soc. 291 L33
[26]	Wang Y and Mukherjee P 2006 Astrophys. J. 650 1
[27]	Eisenstein D J, Zehavi I, Hogg D W, et al. 2005 Astrophys. J. 633 560
[28]	Komatsu E, Smith K M, Dunkley J, et al. 2011 Astrophys. J. Suppl. 192 18
[29]	Amanullah R, Lidman C, Rubin D, et al. 2010 Astrophys. J. 716 712
[30]	Percival W J, Reid B A, Eisenstein D J, et al. 2010 Mon. Not. Roy. Astron. Soc. 401 2148
[31]	Nesseris S and Perivolaropoulos L 2005 Phys. Rev. D 72 123519
[32]	Perivolaropoulos L 2005 Phys. Rev. D 71 063503
[33]	Nesseris S and Perivolaropoulos L 2007 J. Cosmol. Astropart. Phys. 0702 025
[34]	Hu W and Sugiyama N 1996 Astrophys. J. 471 542
[35]	Bond J R, Efstathiou G and Tegmark M 1997 Mon. Not. Roy. Astron. Soc. 291 L33
[36]	Eisenstein D J and Hu W 1998 Astrophys. J. 496 605

New initial condition of the new agegraphic dark energy model

New initial condition of the new agegraphic dark energy model

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