Cosmic Graviton Background and Primordial Gravitational Waves

  • #1
windy miller
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I understand inflation is thought to predict primordial gravitational waves although their strength is undetermined by the theory with some models of inflation predicting them to be strong and others so weak they can never be detected.
However , this paper claims that if we detect a background of cosmic gravitons then all models of inflation would be ruled out. https://arxiv.org/pdf/2208.14088.pdf
Can someone explain why primordial gravitational wave would not also make a cosmic graviton background? Why would detecting this background rue out inflation as a paradigm?
 
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  • #2
I have not yet read through the paper in detail, but I believe there might be an issue of terminology here. As I understand it, "primordial gravitational waves" means gravitational waves produced at the end of inflation due to tiny inhomogeneities in the reheating process (which would also cause fluctuations of other kinds). "Cosmic gravitons", OTOH, according to the paper, means gravitational fluctuations produced before inflation. The paper's basic argument seems to be that the latter kind of gravitational fluctuations would be smoothed by inflation the same way any other kind of fluctuations before inflation would be smoothed, so they would not be detectable once inflation had ended. But that's not the same thing as saying that there would be no fluctuations at all at the end of inflation; the end of inflation itself can produce fluctuations, as described above, and those could include gravitational waves.
 
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  • #3
thanks
 
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FAQ: Cosmic Graviton Background and Primordial Gravitational Waves

What is the Cosmic Graviton Background (CGB)?

The Cosmic Graviton Background (CGB) refers to a hypothetical background of gravitons, which are the theoretical quantum particles that mediate the force of gravity. This background is believed to have been created in the early universe, shortly after the Big Bang, and would carry information about the universe's earliest moments, much like the Cosmic Microwave Background (CMB) does for electromagnetic radiation.

How are Primordial Gravitational Waves generated?

Primordial Gravitational Waves are thought to be generated during the inflationary period of the early universe, a rapid expansion that occurred fractions of a second after the Big Bang. These waves are ripples in spacetime caused by quantum fluctuations that were stretched to macroscopic scales by inflation. They carry information about the energy scales and dynamics of the inflationary period.

What is the significance of detecting Primordial Gravitational Waves?

Detecting Primordial Gravitational Waves would provide direct evidence for the theory of inflation and offer insights into the physics of the early universe, including the energy scales involved. It would also help in understanding the fundamental forces and particles that governed the universe's birth and evolution.

What methods are used to detect the Cosmic Graviton Background and Primordial Gravitational Waves?

Detection methods for Primordial Gravitational Waves primarily involve observing the polarization patterns in the Cosmic Microwave Background (CMB) radiation, particularly the B-mode polarization. Advanced observatories like the Laser Interferometer Gravitational-Wave Observatory (LIGO) and the future space-based Laser Interferometer Space Antenna (LISA) aim to detect these waves directly. The Cosmic Graviton Background, being hypothetical, would require new and highly sensitive technologies to detect, as gravitons interact very weakly with matter.

What challenges are faced in detecting the Cosmic Graviton Background and Primordial Gravitational Waves?

The primary challenges include the extremely weak signal of these gravitational waves and the need for highly sensitive instruments to detect them. Background noise from various astrophysical sources and the need to separate the primordial signals from other gravitational wave sources add to the complexity. Moreover, the theoretical nature of gravitons makes their detection even more challenging, requiring advancements in both theoretical models and experimental technologies.

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