CMB 与超标准宇宙学模型 郭宗宽 非线性和引力及时间本质研讨会，宁波大学

内容 一．宇宙微波背景辐射（ CMB ）物理起源 二． Planck 之后的标准宇宙学模型 三． Planck 之后的一些问题 Big Bang Universe

一. CMB 物理起源 Mather, Smoot 1989 Wilson, Penzias 1964

COBE yrWMAP yrPlanck mo NASA: CMBPol ESA: COrE COBE WMAP9Planck 2013

Ground-based experiments ACBAR, CBI, VSA, QUaD, … ACT, ACTPol (2013~) SPT, SPTpol (95,150GHz, 2012~2015), SPT-3G (2016~2019) BICEP1 (2006~2008), BICEP2 (150GHz, 2010~2012), BICEP3 (95GHz, 2016~) POLARBEAR (150GHz, 2012~2013), POLARBEAR-2 (95,150GHz, 2016~) GroundBIRD (145,220GHz, 2016~) QUBIC (r ~ 0.01, bolometer, interferometer) Balloon-borne experiments BOOMRANG, MAXIMA, … EBEX (150,250,410GHz, 2012), EBEX6K (90,150,220,280GHz, 2018) SPIDER (94,150,280GHz, 2013/2015) PIPER (200,270,350,600GHz, 2015)

二. Planck 之后的标准宇宙学模型 1. 六参数标准宇宙学模型 2.Planck 对标准宇宙学模型的限制 Launched on 14 May 2009 Work for 30 months Complete 5 full-sky surveys Planck 2013 results released 20 Mar 2013, 31 papers Planck 2013 results. XVI, cited by 2775 records Planck 2014 results presented at a conference, 1-5 Dec 2014 Planck 2014 results will be released before the end of

– 宇宙晚期的 4 个参数： – 宇宙早期的 2 个参数： 1. 六参数标准宇宙学模型 V ( ϕ ) ϕ inflation 1981 reheating

2. Planck 对标准宇宙学模型的限制 相比 WMAP ， Planck 的优势： ① high sensitivity ② wide frequency – Planck: 30,44,70,100,143,217,353,545,857 GHz – WMAP: 23,33,41,61,94 GHz ③ high resolution ~ 5′ (WMAP: 15′) PlanckWMAP9 TT

“None of these models are favoured over the standard six-parameter ΛCDM cosmology.” 标准宇宙学手册

Ferrara_Dec1_16h30_Efstathiou_Cosmology.pdf

三. Planck 之后的一些问题

1. 宇宙晚期的膨胀历史 11 Planck Collaboration, “Planck 2013 results. XVI. Cosmological parameters”, arXiv:

RG Cai, ZK Guo, B Tang, Phys. Rev. D89 (2014) about 1.4  discrepancy

2. 宇宙晚期的结构形成 1σ1σ Planck Collaboration, “Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts”, arXiv:

JW Hu, RG Cai, ZK Guo, B Hu, JCAP 05 (2014) 020.

3. 宇宙早期的原初扰动 – Planck 温度涨落的反常： power deficit at low-l, hemispherical asymmetry, the quadrupole-octopole alignment, parity asymmetry, the cold spot Planck Collaboration, “Planck 2013 results. XXIII. Isotropy and statistics of the CMB”, arXiv:

the Sachs-Wolfe effect the diploe modulation of curvature perturbation the asymmetry A is For a single-field slow-roll inflation,

bounce inflation: For the bounce inflation, ZG Liu, ZK Guo, YS Piao, Phys. Rev. D88 (2013) ; ZG Liu, ZK Guo, YS Piao, EPJC 74 (2014) 3006.

Planck Collaboration, “Planck 2013 results. XXII. Constraints on inflation”, arXiv: Observable gravity waves imply inflation happened around the GUT scale. Observable gravity waves imply super- Planckian field excursion.

ZK Guo, N. Ohta, S. Tsujikawa, Phys. Rev. D75 (2007) ; ZK Guo, D.J. Schwarz, Phys. Rev. D80 (2009) ; ZK Guo, D.J. Schwarz, Phys. Rev. D81 (2010) inflation with the Gauss-Bonnet coupling: background equations in a spatially-flat FRW Universe: introducing Hubble and GB flow parameters:

a)The scalar spectral index contains not only the Hubble but also GB flow parameters. b)The degeneracy of standard consistency relation is broken. c)the horizon-crossing time

PX Jiang, JW Hu, ZK Guo, Phys. Rev. D88 (2013)  chaotic inflation with an inverse power-law coupling  chaotic inflation with a dilaton-like coupling

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