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  • WordNet 3.6
    • n CMBR (cosmology) the cooled remnant of the hot big bang that fills the entire universe and can be observed today with an average temperature of about 2.725 kelvin
    • ***


In science:

Particles of EG origin and energies above ≈ 5 · 1019 eV loose a large fraction of their energies due to interactions with CMBR .
Grand Unification Signal from Ultra High Energy Cosmic Rays?
Thus, by imposing the condition of Zel’dovich specra (nS − 1 ≃ 0 ≃ nT ) which is consistent with the CMBR observation, we can derive constraints on ǫi ’s, thus on the parameters of the gravity theory (V, ω, and F ).
Inflationary spectra in generalized gravity: Unified forms
CMBR (e.g., MAP, Planck) are designed to obtain a wealth of valuable data.
Einstein's Biggest Blunder? High-Redshift Supernovae and the Accelerating Universe
The use of observational data on CMBR, large scale structure (LSS), SNIa and Hubble parameter measurements from the Hubble Space Telescope (HST) under the assumption of the redshift independent parameter w give the restriction −1.38 < w < −0.82 at the 95% confidence level .
Generalized phantom energy
Its observation will play a significant role in a foreseeable future for detection of gravitational waves of cosmological origin by CMBR-radiometry space missions [112].
General Relativistic Theory of Light Propagation in the Field of Radiative Gravitational Multipoles
Recent observations of cosmic microwave background radiation (CMBR) by the Wilkinson Microwave Anisotropy Probe (WMAP) experiment and of the large scale structure by redshift surveys e.g the Sloan Digital Sky Survey (SDSS) and the 2-Degree Field (2df ) redshift survey have further strengthened this result.
Reconstructing K-essence
Gravitons can propagate through the expanding universe, living prints on the power spectrum and polarization of the cosmic microwave background radiation (CMBR).
Gravitational Waves generated during inflation from a 5D vacuum theory of gravity in a de Sitter expansion
SNe Ia and CMBR favor accelerating models (q < 0), but they do not altogether rule out the decelerating ones which are also consistent with these observations.
Bianchi Type V Matter Filled Universe with Varying Lambda Term in General Relativity
Physical Review D, 71, 043501, 2005. Andrade, A. P.; Wuensche, C. A.; Ribeiro, A.L.B. Contribution of a mixed mixture model to the anisotropies of the CMBR.
25 years of Cosmic Microwave Background research at INPE
This relic radiation from the Big-Bang has been cooling since then and presently permeates the whole cosmos with a microwave background radiation (CMBR) of temperature T ≃ 3 K.
Cosmic Magnetic Fields: from Stars and Galaxies to the Primordial Universe
Both the CMBR and the Big-Bang nucleosynthesis (BBN) impose constraints on the strength of primordial fields (e.g., ; ).
Cosmic Magnetic Fields: from Stars and Galaxies to the Primordial Universe
In the case of the CMBR, the existence of a strong magnetic field a t the recombination era would have affected it through two effects: (i) breaking the spatial isotropy; and (ii) producing MHD alterations on the temperature and polarization fluctuations of the CMBR.
Cosmic Magnetic Fields: from Stars and Galaxies to the Primordial Universe
These fluctuations have been imprinted on the CMBR by pr imordial density fluctuations (probably produced in the Universe right after the B-B, during the in flation phase, and later on allowed the formation of the large structures in the Universe).
Cosmic Magnetic Fields: from Stars and Galaxies to the Primordial Universe
The lack of these effects on the CMBR implies an upper limit on the background magnetic field at the present Universe Bo < 10−8 − 10−9 G.
Cosmic Magnetic Fields: from Stars and Galaxies to the Primordial Universe
Thus, these upper limits derived from the CMBR and BBN constrain the present cosmic magnetic field to values that are consistent with the inferred values for the IGM today (10−9 G.).
Cosmic Magnetic Fields: from Stars and Galaxies to the Primordial Universe