Large angular scale CMB anisotropy from an excited initial mode

A. Sojasi; M. Mohsenzadeh; E. Yusofi

doi:10.1088/1674-1137/40/7/075101

Chinese Physics C> 2016, Vol. 40> Issue(7) : 075101 DOI: 10.1088/1674-1137/40/7/075101

Large angular scale CMB anisotropy from an excited initial mode

A. Sojasi ^1,, ,
M. Mohsenzadeh ^2,, ,
E. Yusofi ^3,,

Abstract
HTML
Reference
Related

PDF

Abstract：
According to inflationary cosmology, the CMB anisotropy gives an opportunity to test predictions of new physics hypotheses. The initial state of quantum fluctuations is one of the important options at high energy scale, as it can affect observables such as the CMB power spectrum. In this study a quasi-de Sitter inflationary background with approximate de Sitter mode function built over the Bunch-Davies mode is applied to investigate the scale-dependency of the CMB anisotropy. The recent Planck constraint on spectral index motivated us to examine the effect of a new excited mode function (instead of pure de Sitter mode) on the CMB anisotropy at large angular scales. In so doing, it is found that the angular scale-invariance in the CMB temperature fluctuations is broken and in the limit l<200 a tiny deviation appears. Also, it is shown that the power spectrum of CMB anisotropy is dependent on a free parameter with mass dimension H<< M_*< M_p and on the slow-roll parameter ε.
- initial state ,
- power spectrum ,
- CMB anisotropy

References

[1]	S. Dodelson, Modern Cosmology (New York:Accademic Press, 2003)
[2]	V. M. Moukhanov, Physical Foundation of Cosmology (New York:Cambridge University Press, 2005)
[3]	S. Weinberg, Cosmology (New York:Cambridge University Press, 2008)
[4]	A. H. Guth, Phys. Rev. D, 23:347(1981)
[5]	D. H. Lyth and A. R. Liddle, The primordial density pertur-bation:cosmology, in ation and the origin of structure (New York:Cambridge University Press, 2009)
[6]	D. Baumann, TASI 2009, arXiv:hep-th/0907.5424v1
[7]	G. Hinshaw, D. Larson, E. Komatsu et al, ApJS, 208:19(2013)
[8]	P. A. R. Ade et al, Astron. Asstrophys. A, 571:22(2014); P. Ade et al[arXiv:1502.02114]
[9]	A. Kempf and J. C. Niemeyer, Phys. Rev. D, 64:103501(2001)
[10]	N. Kaloper et al, Phys. Rev. D, 66:123510(2002)
[11]	U. H. Danielsson, Phys. Rev. D, 66:023511(2002)
[12]	J. Martin and R. H. Brandenberger, Phys. Rev. D, 68:063513(2003)
[13]	A. Ashoorioon et al, JCAP, 02:025(2014)
[14]	R. Holman and A. J. Tolley, JCAP, 05:001(2008)
[15]	S. Kundu, JCAP, 02:005(2012)
[16]	S. Kundu, arXiv:1311.1575v1
[17]	T. S. Bunch and P. C. W. Davies, Proc. Roy. Soc. Lond. A, 360:117(1978)
[18]	Y. Cai, Y. Wang, and Y. Piao, Phys. Rev D, 92:023518(2015)
[19]	Y. Cai, T. Qiu, J. Xia, and X. Zhang, Phys. Rev. D, 79:021303(2009)
[20]	Y. Cai, D. A. Easson, and R. Brandenberger, JCAP, 08:020(2012)
[21]	J. Xia, Y. Cai, H. Li, and X. Zhang, Phys. Rev. Lett., 112:251301(2014)
[22]	Y. Cai, SCIENCE CHINA, Physics, Mechanics and Astronomy, 57:1414(2014)
[23]	Y. Piao, B. Feng, and X. Zhang, Phys. Rev. D, 69:103520(2004)
[24]	Z. Liu, Z. Guo, and Y. Piao, Eur. Phys. J. C, 74:3006(2014)
[25]	Z. Liu, Z. Guo, and Y. Piao, Phys. Rev. D, 88:063539(2013)
[26]	Y. Wang and Y. Piao, arXiv:gr-qc/1409.7153v3
[27]	R. H. Brandenberger, arXiv:hep-ph/9910410
[28]	J. Martin and R. H. Brandenberger, Phys. Rev. D, 63:123501(2001)
[29]	Y. Cai and Y. Wang, Phys. Let. B, 735:108111(2014)
[30]	Y. Cai, F. Chen, E. G. M. Ferreira, and J. Quintin, arXiv:1412.4298[hep-th]
[31]	Y. Cai, E. G. M. Ferreira, B. Hu, and J. Quintin, Phys. Rev. D, 92:121303(2015)
[32]	E. Yusofiand M. Mohsenzadeh, Phys. Let. B, 735:261265(2014)
[33]	M. Mohsenzadeh, M. R. Tanhayi, and E. Yusofi, Eur. Phys. J. C, 74:2920(2014)
[34]	E. Yusofiand M. Mohsenzadeh, Mod. Phys. Lett. A, 30:1550041(2015)
[35]	M. Mohsenzadeh, E. Yusofi, and M. R. Tanhayi, Canadian Journal of Physics, 93:14661469(2015)
[36]	E. Yusofiand M. Mohsenzadeh, JHEP, 09:020(2014)
[37]	C. Caroll, SPACE TIME AND GEOMETRY An introduction to general relativity (Sanfrancisco:Addition Wesley, 2003)
[38]	N. D. Birrel, P.C.W. Davies, Quantum Field in Curved Space-time (Cambridge, Cambridge University Press, 1982)
[39]	L Bergstrom U. H. Danielsson, JHEP, 0212:038(2002)
[40]	I. S. Gradshteyn and I. M. Ryzhik, Table of Integrals,Series and Products (Elsevier Accademic Press, 2007)
[41]	P. A. R. Ade et al, arxiv:astro-ph/1303.5083
[42]	Y. Cai, W. Zhao, and Y. Zhang, Phys. Rev. D, 89:023005(2014)

[1]	Renli Xu , Chen Wu , Jian Liu , Bin Hong , Jie Peng , Xiong Li , Ruxian Zhu , Zhizhen Zhao , Zhongzhou Ren . Ground-state properties of finite nuclei in relativistic Hartree-Bogoliubov theory with an improved quark mass density-dependent model. Chinese Physics C, 2026, 50(2): 1-12.
[2]	. Correlation between Zero-Sound modes and nuclear equation of state stiffness detected by light vector boson. Chinese Physics C, 2026, 50(1): 014101. doi: 10.1088/1674-1137/adfa81
[3]	. Testing Einstein-Maxwell Power-Yang-Mills hair via black hole photon rings. Chinese Physics C, 2026, 50(1): 015101. doi: 10.1088/1674-1137/ae039c
[4]	M. Zubair , Hira Sohail , Saira Waheed , Amara Ilyas , Irfan Mahmood . Stellar Configurations in f(R, L_m, T) Gravity: Probing Anisotropy and Stability via Minimal Geometric Deformation. Chinese Physics C, 2026, 50(2): 1-21.
[5]	. Bayesian and Monte Carlo approaches to estimating uncertainty for the measurement of the bound-state β^- decay of ²⁰⁵Tl⁸¹⁺. Chinese Physics C, 2025, 49(11): 114001. doi: 10.1088/1674-1137/ade956
[6]	Erdem Sucu , İzzet Sakallı . Quantum tunneling and Aschenbach effect in nonlinear Einstein-Power-Yang-Mills AdS black holes. Chinese Physics C, 2025, 49(10): 105101. doi: 10.1088/1674-1137/add8fe
[7]	Xiaobin Wang , Lei Chang . Unveiling the inner structure of the Pion’s first excited state. Chinese Physics C, 2025, 49(12): 123107. doi: 10.1088/1674-1137/adfc34
[8]	ZHANG Da-Lin , QIU Sui-Zheng , LIU Chang-Liang , SU Guang-Hui . Steady state investigation on neutronics of a molten salt reactor considering the flow effect of fuel salt. Chinese Physics C, 2008, 32(8): 624-628. doi: 10.1088/1674-1137/32/8/007

Access

Get Citation

A. Sojasi, M. Mohsenzadeh and E. Yusofi. Large angular scale CMB anisotropy from an excited initial mode[J]. Chinese Physics C, 2016, 40(7): 075101. doi: 10.1088/1674-1137/40/7/075101

A. Sojasi, M. Mohsenzadeh and E. Yusofi. Large angular scale CMB anisotropy from an excited initial mode[J]. Chinese Physics C, 2016, 40(7): 075101. doi: 10.1088/1674-1137/40/7/075101 shu

RIS(for EndNote,Reference Manager,ProCite)

BibTex

Txt

Milestone

Received: 2015-12-22
Revised: 2015-03-01

Fund

Supported by the Islamic Azad University, Rasht Branch, Rasht, Iran

Article Metric

Article Views(3225)
PDF Downloads(267)
Cited by(0)

Policy on re-use

To reuse of subscription content published by CPC, the users need to request permission from CPC, unless the content was published under an Open Access license which automatically permits that type of reuse.

通讯作者: 陈斌, bchen63@163.com

1.
沈阳化工大学材料科学与工程学院沈阳 110142

Large angular scale CMB anisotropy from an excited initial mode

Corresponding author: A. Sojasi,

Corresponding author: M. Mohsenzadeh,

Corresponding author: E. Yusofi,

Received Date: 2015-12-22

Accepted Date: 2015-03-01

Available Online: 2016-07-05

Fund Project: Supported by the Islamic Azad University, Rasht Branch, Rasht, Iran

Abstract: According to inflationary cosmology, the CMB anisotropy gives an opportunity to test predictions of new physics hypotheses. The initial state of quantum fluctuations is one of the important options at high energy scale, as it can affect observables such as the CMB power spectrum. In this study a quasi-de Sitter inflationary background with approximate de Sitter mode function built over the Bunch-Davies mode is applied to investigate the scale-dependency of the CMB anisotropy. The recent Planck constraint on spectral index motivated us to examine the effect of a new excited mode function (instead of pure de Sitter mode) on the CMB anisotropy at large angular scales. In so doing, it is found that the angular scale-invariance in the CMB temperature fluctuations is broken and in the limit l<200 a tiny deviation appears. Also, it is shown that the power spectrum of CMB anisotropy is dependent on a free parameter with mass dimension H<< M_*< M_p and on the slow-roll parameter ε.

HTML

Reference (42)

Large angular scale CMB anisotropy from an excited initial mode

Abstract：

References

Access

Article Metrics

Metrics

通讯作者: 陈斌, bchen63@163.com

Email This Article