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Can LIGO Detect A Graviton?

A lecture given 10/27/08 by Professor Freeman Dyson of the Institute of Advanced Studies at Princeton, in honor of the 100th anniversary of the founding of the University of California, Davis. $$E=\left(\frac{c^{2}}{32\pi G}\right)\omega^{2}f^{2}$$ is the energy per gravity wave, where f is the dimensionless amplitude/strain. $$E_{s}=\frac{\hbar\omega^{4}}{c^{3}}$$ is the energy per graviton, taken from $\hbar\omega$ energy times $\frac{\omega^3}{c^3}$ density $$f=\left(32\pi\right)^{\frac{1}{2}}\left(L_{p}\frac{\omega}{c}\right)$$ is the strain per graviton. $$L_{p}=\left(\frac{G\hbar}{c^{3}}\right)^{\frac{1}{2}}=1.4\times10^{-33}cm$$ $$\delta=\left(32\pi\right)^{\frac{1}{2}}L_{p}$$ Gives the linear displacement per graviton.



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Can LIGO Detect A Graviton?

https://adamgetchell.org/posts/can-ligo-detect-graviton

A lecture given 10/27/08 by Professor Freeman Dyson of the Institute of Advanced Studies at Princeton, in honor of the 100th anniversary of the founding of the University of California, Davis. $$E=\left(\frac{c^{2}}{32\pi G}\right)\omega^{2}f^{2}$$ is the energy per gravity wave, where f is the dimensionless amplitude/strain. $$E_{s}=\frac{\hbar\omega^{4}}{c^{3}}$$ is the energy per graviton, taken from $\hbar\omega$ energy times $\frac{\omega^3}{c^3}$ density $$f=\left(32\pi\right)^{\frac{1}{2}}\left(L_{p}\frac{\omega}{c}\right)$$ is the strain per graviton. $$L_{p}=\left(\frac{G\hbar}{c^{3}}\right)^{\frac{1}{2}}=1.4\times10^{-33}cm$$ $$\delta=\left(32\pi\right)^{\frac{1}{2}}L_{p}$$ Gives the linear displacement per graviton.



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https://adamgetchell.org/posts/can-ligo-detect-graviton

Can LIGO Detect A Graviton?

A lecture given 10/27/08 by Professor Freeman Dyson of the Institute of Advanced Studies at Princeton, in honor of the 100th anniversary of the founding of the University of California, Davis. $$E=\left(\frac{c^{2}}{32\pi G}\right)\omega^{2}f^{2}$$ is the energy per gravity wave, where f is the dimensionless amplitude/strain. $$E_{s}=\frac{\hbar\omega^{4}}{c^{3}}$$ is the energy per graviton, taken from $\hbar\omega$ energy times $\frac{\omega^3}{c^3}$ density $$f=\left(32\pi\right)^{\frac{1}{2}}\left(L_{p}\frac{\omega}{c}\right)$$ is the strain per graviton. $$L_{p}=\left(\frac{G\hbar}{c^{3}}\right)^{\frac{1}{2}}=1.4\times10^{-33}cm$$ $$\delta=\left(32\pi\right)^{\frac{1}{2}}L_{p}$$ Gives the linear displacement per graviton.

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      A lecture given 10/27/08 by Professor Freeman Dyson of the Institute of Advanced Studies at Princeton, in honor of the 100th anniversary of the founding of the University of California, Davis. $$E=\left(\frac{c^{2}}{32\pi G}\right)\omega^{2}f^{2}$$ is the energy per gravity wave, where f is the dimensionless amplitude/strain. $$E_{s}=\frac{\hbar\omega^{4}}{c^{3}}$$ is the energy per graviton, taken from $\hbar\omega$ energy times $\frac{\omega^3}{c^3}$ density $$f=\left(32\pi\right)^{\frac{1}{2}}\left(L_{p}\frac{\omega}{c}\right)$$ is the strain per graviton. $$L_{p}=\left(\frac{G\hbar}{c^{3}}\right)^{\frac{1}{2}}=1.4\times10^{-33}cm$$ $$\delta=\left(32\pi\right)^{\frac{1}{2}}L_{p}$$ Gives the linear displacement per graviton.

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      A lecture given 10/27/08 by Professor Freeman Dyson of the Institute of Advanced Studies at Princeton, in honor of the 100th anniversary of the founding of the University of California, Davis. $$E=\left(\frac{c^{2}}{32\pi G}\right)\omega^{2}f^{2}$$ is the energy per gravity wave, where f is the dimensionless amplitude/strain. $$E_{s}=\frac{\hbar\omega^{4}}{c^{3}}$$ is the energy per graviton, taken from $\hbar\omega$ energy times $\frac{\omega^3}{c^3}$ density $$f=\left(32\pi\right)^{\frac{1}{2}}\left(L_{p}\frac{\omega}{c}\right)$$ is the strain per graviton. $$L_{p}=\left(\frac{G\hbar}{c^{3}}\right)^{\frac{1}{2}}=1.4\times10^{-33}cm$$ $$\delta=\left(32\pi\right)^{\frac{1}{2}}L_{p}$$ Gives the linear displacement per graviton.
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      A lecture given 10/27/08 by Professor Freeman Dyson of the Institute of Advanced Studies at Princeton, in honor of the 100th anniversary of the founding of the University of California, Davis. $$E=\left(\frac{c^{2}}{32\pi G}\right)\omega^{2}f^{2}$$ is the energy per gravity wave, where f is the dimensionless amplitude/strain. $$E_{s}=\frac{\hbar\omega^{4}}{c^{3}}$$ is the energy per graviton, taken from $\hbar\omega$ energy times $\frac{\omega^3}{c^3}$ density $$f=\left(32\pi\right)^{\frac{1}{2}}\left(L_{p}\frac{\omega}{c}\right)$$ is the strain per graviton. $$L_{p}=\left(\frac{G\hbar}{c^{3}}\right)^{\frac{1}{2}}=1.4\times10^{-33}cm$$ $$\delta=\left(32\pi\right)^{\frac{1}{2}}L_{p}$$ Gives the linear displacement per graviton.

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      Can LIGO Detect A Graviton?
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      A lecture given 10/27/08 by Professor Freeman Dyson of the Institute of Advanced Studies at Princeton, in honor of the 100th anniversary of the founding of the University of California, Davis. $$E=\left(\frac{c^{2}}{32\pi G}\right)\omega^{2}f^{2}$$ is the energy per gravity wave, where f is the dimensionless amplitude/strain. $$E_{s}=\frac{\hbar\omega^{4}}{c^{3}}$$ is the energy per graviton, taken from $\hbar\omega$ energy times $\frac{\omega^3}{c^3}$ density $$f=\left(32\pi\right)^{\frac{1}{2}}\left(L_{p}\frac{\omega}{c}\right)$$ is the strain per graviton. $$L_{p}=\left(\frac{G\hbar}{c^{3}}\right)^{\frac{1}{2}}=1.4\times10^{-33}cm$$ $$\delta=\left(32\pi\right)^{\frac{1}{2}}L_{p}$$ Gives the linear displacement per graviton.
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