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Peaks in the CMBR power spectrum: Physical interpretation for any cosmological scenario Martín López-Corredoira Instituto de Astrofísica de Canarias Tenerife,

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Presentation on theme: "Peaks in the CMBR power spectrum: Physical interpretation for any cosmological scenario Martín López-Corredoira Instituto de Astrofísica de Canarias Tenerife,"— Presentation transcript:

1 Peaks in the CMBR power spectrum: Physical interpretation for any cosmological scenario Martín López-Corredoira Instituto de Astrofísica de Canarias Tenerife, Spain References: López-Corredoira & Gabrielli, 2013, Physica A, 392, 474 López-Corredoira, 2013, Int. J. Mod. Phys. D, 22(7), id

2 Two-point correlation function (Transform: Fourier/Legendre) Power spectrum Origin of the oscillations

3 Origin of the oscillations

4 How to generate abrupt changes in the correlation function? Toy Model Filled disks of contant radius R=1 o with a Poissonian distribution

5 How to generate abrupt changes in the correlation function? Toy Model Filled disks of contant radius R=1 o with a random distribution but disks do not intersect

6 How to generate abrupt changes in the correlation function? Toy Model Filled disks of contant radius R=1 o with a non- Poissonian distribution

7 How to generate abrupt changes in the correlation function? Toy Model Filled disks of variable (finite) radius with any distribution inside, and distribution of disks

8 A model to generate CMBR power spectrum Physical interpretation Disks may represent a projection of spherical regions in 3D space. The standard cosmological model is a particular case in which the radius of the disk is constant representing the size of the acoustic horizon (diameter of the acoustic horizon region at recombination epoch: 1.2 degrees). Photon-baryon fluid compressed by gravitational attraction produced by local density fluctuations. Non-standard cosmological models: any fluid with clouds of overdensities that emits/absorbs radiation or interact gravitationally with the photons. Different radii is possible when the 3D distribution projects clouds from different distances.

9 Caveats of an alternative model of CMBR Physical interpretation Black body shape. (Almost) Gaussian fluctuations. Only 6 free parameters to fit the power spectrum.

10 WMAP-7yr data How many free Parameters? f 6 : set of polynomial functions with continuous derivative with 6 free parameters: χ red 2 =3.0 f 4 : set of polynomial functions with continuous derivative with 4 free parameters. g 4 : set of polynomial / logarithmic functions with 4 free parameters. Dip = anticorrelation of disks

11 WMAP-7yr + ATACAMA/ACT data How many free Parameters? f 6,A : set of polynomial functions with continuous derivative with 6 free parameters: χ red 2 =1.4

12 Power spectrum How many free Parameters? Peaks 3rd. and beyond are not fitted with the sets of polynomials (possibly because we have not used ѳ <0.2 deg.)

13 Power spectrum How many free Parameters? Narlikar et al. (2007): WMAP-3yr data. Solid line: QSSC and clusters of galaxies with 6 parameters; Dashed line: standard model. Angus & Diaferio (2011): WMAP-7yr+ACT+ACBAR data. Blue line: MOND, with sterile neutrinos with 6 free parameters; Red line: standard model.

14 Discussion Success of standard cosmological model? Succesful predictions: 1.Isotropy 2.Black body radiation 3.Peaks in CMBR power spectrum (Peebles & Yu 1970) Etc. Wrong predictions which were corrected ad hoc: 1.Temperature T CMBR =50 K (Gamow 1961) or 30 K (Dicke et al. 1965) 2.Amplitude of the anisotropies ( ΔT/T ~ ; Sachs & Wolfe 1967) 3.Position of the first peak at l200 (measured for the first time in the middle 90s [White et al. 1996] and contradicting the preferred cosmological model at that time= m 0.2) 4.Amplitude of the second peak as high as the first peak (Bond & Efstathiou 1987) Etc. Dark matter ad hoc Dark energy ad hoc

15 Discussion General features of CMBR and its power spectrum/two-point correlation function: 1.Temperature T CMBR =3 K 2.Isotropy 3.Black body radiation 4.Gaussian fluctuations 5.Peaks in CMBR power spectrum 6.6 free parameters should fit it 7.Others (polarization,…) Explanations which do not require the standard model: Several ideas (e.g., stellar radiation) Radiation coming from all directions Thermalization of radiation? Not clear yet There are many processes in Nature which generate Gaussian fluctuations; but, there may be non-Gaussianity too Abrupt transition of emission/absorption inside and outside some clouds/regions A simple set of polynomials produce a quite good fit of the 2-point corr.func., but do not explain 3rd peak 2nd peak amplitude FURTHER RESEARCH IS NEEDED Pending Recipe to cook CMBR in an alternative cosmology Major problem References: López-Corredoira & Gabrielli, 2013, Physica A, 392, 474 López-Corredoira, 2013, Int. J. Mod. Phys. D, 22(7), id

16 Science is in decline. Facts and challenging ideas about the exhaustion of our culture in The Twilight of the Scientific Age Publisher: BrownWalker Press Year: 2013 Book available at: BrownWalker Press, Amazon, Barnes & Noble,…


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