Density fluctuations in $\kappa$-deformed inflationary universe

Chaiho Rim; Hyeong-Chan Kim; Jae Hyung Yee

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Density fluctuations in $\kappa$-deformed inflationary universe

Hyeong-Chan Kim, Jae Hyung Yee, Chaiho Rim

General Relativity and Quantum Cosmology · Submitted 27 Jun 2005

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The authors' main claim We show that the power spectra of the metric fluctuation have non-trivial corrections on the time dependence and on the momentum dependence compared to the commutative space results.

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arXiv IDgr-qc/0506122 (version 3)

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CitationChaiho Rim, Hyeong-Chan Kim, Jae Hyung Yee. "Density fluctuations in $\kappa$-deformed inflationary universe." arXiv:gr-qc/0506122 (2005). https://pith.science/paper/OMVSEZQJ

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.20 · human participants 0.01 · controlled comparison 0.26 · randomized assignment 0.01 · states quantitative result 0.47 · compares with prior results 0.84 · mentions code or data availability 0.02.

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arXiv listing abstract v3. Results and the main claim are underlined; show every role.

We study the spectrum of metric fluctuation in $\kappa$-deformed inflationary universe. We write the theory of scalar metric fluctuations in the $\kappa-$deformed Robertson-Walker space, which is represented as a non-local theory in the conventional Robertson-Walker space. One important consequence of the deformation is that the mode generation time is naturally determined by the structure of the $\kappa-$deformation. We expand the non-local action in $H^2/\kappa^2$, with $H$ being the Hubble parameter and $\kappa$ the deformation parameter, and then compute the power spectra of scalar metric fluctuations both for the cases of exponential and power law inflations up to the first order in $H^2/\kappa^2$. We show that the power spectra of the metric fluctuation have non-trivial corrections on the time dependence and on the momentum dependence compared to the commutative space results. Especially for the power law inflation case, the power spectrum for UV modes is weakly blue shifted early in the inflation and its strength decreases in time. The power spectrum of far-IR modes has cutoff proportional to $k^3$ which may explain the low CMB quadrupole moment.

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What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We study the spectrum of metric fluctuation in $\kappa$-deformed inflationary universe.	contribution 0.99	0.93	0.04	asserted 0.63
s1	We write the theory of scalar metric fluctuations in the $\kappa-$deformed Robertson-Walker space, which is represented as a non-local theory in the conventional Robertson-Walker space.	method 0.77	0.92	0.05	asserted 1.00
s2	One important consequence of the deformation is that the mode generation time is naturally determined by the structure of the $\kappa-$deformation.	result 0.57	0.66	0.17	asserted 1.00
s3	We expand the non-local action in $H^2/\kappa^2$, with $H$ being the Hubble parameter and $\kappa$ the deformation parameter, and then compute the power spectra of scalar metric fluctuations both for the cases of exponential and power law inflations up to the first order in $H^2/\kappa^2$.	method 0.98	0.96	0.10	asserted 0.96
s4	We show that the power spectra of the metric fluctuation have non-trivial corrections on the time dependence and on the momentum dependence compared to the commutative space results.	result 1.00	0.95	0.53	asserted 1.00
s5	Especially for the power law inflation case, the power spectrum for UV modes is weakly blue shifted early in the inflation and its strength decreases in time.	result 1.00	0.93	0.17	asserted 1.00
s6	The power spectrum of far-IR modes has cutoff proportional to $k^3$ which may explain the low CMB quadrupole moment.	interpretation 0.51	0.89	0.23	hedged possibility 0.99

What kind of paper the classifier reports this is: theoretical result 1.00 · evidence from proof or derivation 0.99.

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The paper

Original abstract

We study the spectrum of metric fluctuation in $\kappa$-deformed inflationary universe. We write the theory of scalar metric fluctuations in the $\kappa-$deformed Robertson-Walker space, which is represented as a non-local theory in the conventional Robertson-Walker space. One important consequence of the deformation is that the mode generation time is naturally determined by the structure of the $\kappa-$deformation. We expand the non-local action in $H^2/\kappa^2$, with $H$ being the Hubble parameter and $\kappa$ the deformation parameter, and then compute the power spectra of scalar metric fluctuations both for the cases of exponential and power law inflations up to the first order in $H^2/\kappa^2$. We show that the power spectra of the metric fluctuation have non-trivial corrections on the time dependence and on the momentum dependence compared to the commutative space results. Especially for the power law inflation case, the power spectrum for UV modes is weakly blue shifted early in the inflation and its strength decreases in time. The power spectrum of far-IR modes has cutoff proportional to $k^3$ which may explain the low CMB quadrupole moment.

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5 arXiv papers cite this in 5 sentences

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Cites it as background 3 papers

There are several attempts to show the effect of the non-commutativity of the spacetime on the cosmological observations [ref] [ref] [ref] .

Trans-Planckian Physics and Non-Commutative Inflation · Introduction · 0.94
Furthermore, scalar metric fluctuations in a $κ$-deformed Robertson-Walker space-time has been studied by constructing a nonlocal scalar field theory in the deformed space-time by generalizing the $κ$-Minkowski field theory to Robertson-Walker space-time [ref] .

Modified Mukhanov-Sasaki equation and primordial perturbations in $\kappa$-deformed non-commutative space-time · Introduction · 0.88
An overview of the work done in particle physics can be obtained from [ref] and for cosmology see e.g. [ref] , and references therein.

Noncommutative Gravity and Quantum Field Theory on Noncommutative Curved Spacetimes · Introduction · 0.99

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