RECORD
Degeneracy Enhancement of Neutron-Antineutron Oscillation in Neutron Star
High Energy Physics - Phenomenology · Submitted 14 May 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The subsequent neutron star heating can put an extremely stringent bound on the baryon number violating cross mass term between neutron and antineutron.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
We explore the fermion oscillation in a degenerate environment. The direct consequence is introducing a Pauli blocking factor $1 - f_i$, where $f_i$ is the phase space distribution function, for each intermediate mass eigenstate during propagation. It is then much easier for a state with larger existing fraction or density to oscillate into other states with less degeneracy while the reversed process is not enhanced. This can significantly modify the oscillation behaviors. We apply this degenerate fermion oscillation to a concrete scenario of neutron-antineutron oscillation in neutron star. It turns out antineutrons receive a standing fraction to annihilate with the environmental neutrons. The subsequent neutron star heating can put an extremely stringent bound on the baryon number violating cross mass term between neutron and antineutron.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We explore the fermion oscillation in a degenerate environment. | contribution 0.89 | 0.76 | 0.03 | asserted 0.62 |
| s1 | The direct consequence is introducing a Pauli blocking factor $1 - f_i$, where $f_i$ is the phase space distribution function, for each intermediate mass eigenstate during propagation. | method 0.65 | 0.63 | 0.05 | asserted 1.00 |
| s2 | It is then much easier for a state with larger existing fraction or density to oscillate into other states with less degeneracy while the reversed process is not enhanced. | interpretation 0.60 | 0.68 | 0.17 | asserted 0.91 |
| s3 | This can significantly modify the oscillation behaviors. | interpretation 0.65 | 0.50 | 0.09 | hedged possibility 0.53 |
| s4 | We apply this degenerate fermion oscillation to a concrete scenario of neutron-antineutron oscillation in neutron star. | contribution 0.82 | 0.86 | 0.05 | asserted 0.98 |
| s5 | It turns out antineutrons receive a standing fraction to annihilate with the environmental neutrons. | result 1.00 | 0.89 | 0.18 | asserted 1.00 |
| s6 | The subsequent neutron star heating can put an extremely stringent bound on the baryon number violating cross mass term between neutron and antineutron. | result 0.59 | 0.81 | 0.80 | asserted 0.94 |
What was examined, and what was not
- arXiv listing abstract v2
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
We explore the fermion oscillation in a degenerate environment. The direct consequence is introducing a Pauli blocking factor $1 - f_i$, where $f_i$ is the phase space distribution function, for each intermediate mass eigenstate during propagation. It is then much easier for a state with larger existing fraction or density to oscillate into other states with less degeneracy while the reversed process is not enhanced. This can significantly modify the oscillation behaviors. We apply this degenerate fermion oscillation to a concrete scenario of neutron-antineutron oscillation in neutron star. It turns out antineutrons receive a standing fraction to annihilate with the environmental neutrons. The subsequent neutron star heating can put an extremely stringent bound on the baryon number violating cross mass term between neutron and antineutron.
Human review
How the literature uses it
1 arXiv paper cite this in 6 sentences
Papers citing it · 4 sentences without a confident label
Contests it 1 paper
-
Our results disagree strongly with the claims in [ref] .
Effects of Neutron-Antineutron Transitions in Neutron Stars · Introduction · contest 0.95
What it cites · 22 sentences without a confident label
Uses the method or tool of 2 papers
-
We implement the heating due to $n n̅$ oscillation in [ref] to simulate the NS temperature evolution.
Minimal Cooling of Neutron Stars: A New Paradigm · Introduction · 0.97
-
Treating the $1 - f$ factor as field strength renormalization, our result can be readily obtained with the quantum kinetics theory [ref] .
Neutrinos from dense environments : Flavor mechanisms, theoretical approaches, observations, and new directions · Introduction · 0.80
Uses data or values from 4 papers
-
To match the corresponding high density $n_n ≈4 ×10^38$ cm$^-3$ [ref] , which is also assumed to be constant inside NS, the difference of chemical potential $μ$ from the neutron mass $m$, $μ-m ≈101.6$ MeV, is much larger than temperature $T$ [ref] .
Neutron stars - cooling and transport · Introduction · 0.98
-
To match the corresponding high density $n_n ≈4 ×10^38$ cm$^-3$ [ref] , which is also assumed to be constant inside NS, the difference of chemical potential $μ$ from the neutron mass $m$, $μ-m ≈101.6$ MeV, is much larger than temperature $T$ [ref] .
Constraints on Phase Transitions in Neutron Star Matter · Introduction · 0.98
-
With a very low internal temperature $T ∼7$ keV at the age of $10^5$ years [ref] , the corresponding neutron Fermi momentum $k_F=(3 π^2 n_n)^1/3$ and chemical potential $μ=√(k_F^2+m^2)$ can be readily derived from the neutron density $n_n$ assuming full degeneracy.
Thermal luminosities of cooling neutron stars · Introduction · 0.94
Compares with 2 papers
-
For a fermion, the creation and annihilation operators anticommute as, ${ a_p_1 i, a_p_2 i^†} = (2 π)^3 δ^(3) (p_2 - p_1)$ [During revision, we notice the same $δ^(3)$ function has also been obtained in [ref] .].
Background-Induced Forces from Dark Relics · Introduction · 0.97
-
For a fermion, the creation and annihilation operators anticommute as, ${ a_p_1 i, a_p_2 i^†} = (2 π)^3 δ^(3) (p_2 - p_1)$ [During revision, we notice the same $δ^(3)$ function has also been obtained in [ref] .].
Neutrino forces in neutrino backgrounds · Introduction · 0.97
Cites as background 5 papers
-
Neutron-Antineutron Oscillation with Degeneracy – Being neutral particles, neutron and antineutron can have cross mass term [ref] .
Neutron-Antineutron Oscillations: Theoretical Status and Experimental Prospects · Introduction · 0.90
-
Previous experiments on $n n̅$ oscillation have primarily focused on the processes happening inside atomic nuclei [ref] or in a vacuum environment [ref] .
Realistic calculations of nuclear disappearance lifetimes induced by neutron-antineutron oscillations · Introduction · 0.86
-
Previous experiments on $n n̅$ oscillation have primarily focused on the processes happening inside atomic nuclei [ref] or in a vacuum environment [ref] .
Search for Neutron-Antineutron Oscillations Using Multiprong Events in Soudan 2 · Introduction · 0.86
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.