Definitions for cosmic microwave background radiation
cos·mic mi·crowave back·ground ra·di·a·tion

Princeton's WordNetRate this definition:0.0 / 0 votes

1. cosmic background radiation, CBR, cosmic microwave background radiation, CMBR, cosmic microwave background, CMBnoun

   (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

ChatGPTRate this definition:0.0 / 0 votes

1. cosmic microwave background radiation

   Cosmic microwave background radiation is the residual heat or electromagnetic radiation left over from the Big Bang event that gave birth to the universe about 13.8 billion years ago. It can be detected virtually anywhere in the universe and appears as a faint background noise or glow of heat. This radiation is at an extremely low temperature, roughly -270.45 degrees Celsius or about 2.73 degrees above absolute zero. It provides crucial evidence about the evolution and structure of the universe, and its discovery was a major confirmation of the Big Bang theory.

WikidataRate this definition:0.0 / 0 votes

1. Cosmic microwave background radiation

   In cosmology, cosmic microwave background radiation is thermal radiation filling the observable universe almost uniformly. With a traditional optical telescope, the space between stars and galaxies is completely dark. However, a sufficiently sensitive radio telescope shows a faint background glow, almost exactly the same in all directions, that is not associated with any star, galaxy, or other object. This glow is strongest in the microwave region of the radio spectrum. The CMB's serendipitous discovery in 1964 by American radio astronomers Arno Penzias and Robert Wilson was the culmination of work initiated in the 1940s, and earned them the 1978 Nobel Prize. Cosmic background radiation is well explained as radiation left over from an early stage in the development of the universe, and its discovery is considered a landmark test of the Big Bang model of the universe. When the universe was young, before the formation of stars and planets, it was denser, much hotter, and filled with a uniform glow from a white-hot fog of hydrogen plasma. As the universe expanded, both the plasma and the radiation filling it grew cooler. When the universe cooled enough, protons and electrons combined to form neutral atoms. These atoms could no longer absorb the thermal radiation, and so the universe became transparent instead of being an opaque fog. Cosmologists refer to the time period when neutral atoms first formed as the recombination epoch, and the event shortly afterwards when photons started to travel freely through space rather than constantly being scattered by electrons and protons in plasma is referred to as photon decoupling. The photons that existed at the time of photon decoupling have been propagating ever since, though growing fainter and less energetic, since the expansion of space causes their wavelength to increase over time. This is the source of the alternative term relic radiation. The surface of last scattering refers to the set of points in space at the right distance from us so that we are now receiving photons originally emitted from those points at the time of photon decoupling.−30

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1. • Cosmic Radiation
   • Cosmology

How to pronounce cosmic microwave background radiation?

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How to say cosmic microwave background radiation in sign language?

Numerology

1. Chaldean Numerology

   The numerical value of cosmic microwave background radiation in Chaldean Numerology is: 9

2. Pythagorean Numerology

   The numerical value of cosmic microwave background radiation in Pythagorean Numerology is: 7

References

1. ^ Princeton's WordNet
   http://wordnetweb.princeton.edu/perl/webwn?s=cosmic microwave background radiation
2. ^ ChatGPT
   https://chat.openai.com
3. ^ Wikidata
   https://www.wikidata.org/w/index.php?search=cosmic microwave background radiation