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Neutron - mirror neutron mixing and neutron stars
High Energy Astrophysical Phenomena · Submitted 30 Dec 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim If $50 \% - 50\%$ proportion between two fractions can be reached asymptotically in time, then the maximum mass of such "maximally mixed stars" should be $\sqrt2$ times smaller than that of ordinary neutron star while the stars exceeding a critical mass value $M^{\rm max}_{NS}/\sqrt2$ should collapse in black holes after certain time.
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The abstract, sentence by sentence
The oscillation of neutrons $n$ into mirror neutrons $n'$, their mass degenerate partners from dark mirror sector, can have interesting implications for neutron stars: an ordinary neutron star could gradually transform into a mixed star consisting in part of mirror dark matter. Mixed stars can be detectable as twin partners of ordinary neutron stars: namely, there can exist compact stars with the same masses but having different radii. For a given equation of state (identical between the ordinary and mirror components), the mass and radius of a mixed star depend on the proportion between the ordinary and mirror components in its interior which in turn depends on its age. If $50 \% - 50\%$ proportion between two fractions can be reached asymptotically in time, then the maximum mass of such "maximally mixed stars" should be $\sqrt2$ times smaller than that of ordinary neutron star while the stars exceeding a critical mass value $M^{\rm max}_{NS}/\sqrt2$ should collapse in black holes after certain time. We evaluate the evolution time and discuss the implications of $n-n'$ transition for the pulsar observations as well as for the gravitational waves from the neutron star mergers and associated electromagnetic signals.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The oscillation of neutrons $n$ into mirror neutrons $n'$, their mass degenerate partners from dark mirror sector, can have interesting implications for neutron stars: an ordinary neutron star could gradually transform into a mixed star consisting in part of mirror dark matter. | background 0.83 | 0.12 | 0.28 | hedged possibility 0.98 |
| s1 | Mixed stars can be detectable as twin partners of ordinary neutron stars: namely, there can exist compact stars with the same masses but having different radii. | interpretation 0.53 | 0.23 | 0.20 | hedged possibility 0.95 |
| s2 | For a given equation of state (identical between the ordinary and mirror components), the mass and radius of a mixed star depend on the proportion between the ordinary and mirror components in its interior which in turn depends on its age. | result 0.56 | 0.29 | 0.11 | asserted 0.99 |
| s3 | If $50 \% - 50\%$ proportion between two fractions can be reached asymptotically in time, then the maximum mass of such "maximally mixed stars" should be $\sqrt2$ times smaller than that of ordinary neutron star while the stars exceeding a critical mass value $M^{\rm max}_{NS}/\sqrt2$ should collapse in black holes after certain time. | result 0.82 | 0.62 | 0.44 | hedged possibility 0.48 |
| s4 | We evaluate the evolution time and discuss the implications of $n-n'$ transition for the pulsar observations as well as for the gravitational waves from the neutron star mergers and associated electromagnetic signals. | contribution 0.99 | 0.89 | 0.08 | asserted 0.81 |
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The paper
Original abstract
The oscillation of neutrons $n$ into mirror neutrons $n'$, their mass degenerate partners from dark mirror sector, can have interesting implications for neutron stars: an ordinary neutron star could gradually transform into a mixed star consisting in part of mirror dark matter. Mixed stars can be detectable as twin partners of ordinary neutron stars: namely, there can exist compact stars with the same masses but having different radii. For a given equation of state (identical between the ordinary and mirror components), the mass and radius of a mixed star depend on the proportion between the ordinary and mirror components in its interior which in turn depends on its age. If $50 \% - 50\%$ proportion between two fractions can be reached asymptotically in time, then the maximum mass of such "maximally mixed stars" should be $\sqrt2$ times smaller than that of ordinary neutron star while the stars exceeding a critical mass value $M^{\rm max}_{NS}/\sqrt2$ should collapse in black holes after certain time. We evaluate the evolution time and discuss the implications of $n-n'$ transition for the pulsar observations as well as for the gravitational waves from the neutron star mergers and associated electromagnetic signals.
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References
How the literature uses it
14 arXiv papers cite this in 30 sentences
Papers citing it · 26 sentences without a confident label
Cites it as support 1 paper
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(A) In fact, $n→n'$ conversion can gradually transform a NS into a mixed star having the core of M matter [ref] .
Baryon Number Violation: From Nuclear Matrix Elements to BSM Physics · Baryon violation in cosmic rays: UHECR and cosmic antinuclei · 0.96
Cites it as background 3 papers
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In this paper, we would like to take a step back from concrete scenarios of baryogenesis, and ask a question: What if DM had BNV interactions?[For other ideas connecting nucleon-number-changing processes with dark sector physics, see e.g. Refs. [ref] .] This opens an interesting possibility of $𝒪(GeV)$ energy release in interactions of DM particles with baryons.
Dark Matter Catalyzed Baryon Destruction · Introduction · 0.84
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Observation of $n→n'$ would have interesting astrophysical implications for extreme energy cosmic rays [ref] and for neutron stars [ref] .
Experimental Search for Neutron to Mirror Neutron Oscillations as an Explanation of the Neutron Lifetime Anomaly · Introduction · 0.92
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Such hybrid models have been already discussed in several cases [ref] , in particular dark matter in the Bose-Einstein condensed phase has been considered in [ref] , showing a softening of the EoS as a consequence of the dark matter presence.
Superfluid dark stars · Introduction · 0.85
What it cites · 57 sentences without a confident label
Uses data or values from 13 papers
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In spite of large errors in the mass determination: $M =( 2.74 ±0.21) M_⊙$ [ref] , already the existence of this pulsar challenges the SLy EoS and demands a rather stiff EoS as in Refs. [ref] .[Though, conservatively thinking, there is $1%$ probability of low enough inclination allowing the pulsar mass below $2M_⊙$ [ref] , so that it can be marginally reconciled also with the Sly EoS.]
Eight New Millisecond Pulsars in NGC 6440 and NGC 6441 · Effects of slow NS to MS transformation · 0.80
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In spite of large errors in the mass determination: $M =( 2.74 ±0.21) M_⊙$ [ref] , already the existence of this pulsar challenges the SLy EoS and demands a rather stiff EoS as in Refs. [ref] .[Though, conservatively thinking, there is $1%$ probability of low enough inclination allowing the pulsar mass below $2M_⊙$ [ref] , so that it can be marginally reconciled also with the Sly EoS.]
The Nuclear Equation of State and Neutron Star Masses · Effects of slow NS to MS transformation · 0.80
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The first event GW170817 [ref] is considered as a clear signal of the ordinary NS merger, with masses of two stars $M_1,2$ compatible with $≃1.4 M_⊙$ and their total mass $M_tot = (2.75 ±0.02) M_⊙$ typical for NS binaries.
GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral · Neutron star mergers and associated signals · 0.94
Cites as support 1 paper
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In addition, no confirmed electromagnetic event has been identified in association with this GW signal which suggests that this event could be originated by the merger of mirror NS [ref] .
Testing merging of Dark Exotic Stars from Gravitational Waves in the Multi-messenger approach · Neutron star mergers and associated signals · 0.97
Cites as background 9 papers
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were briefly discussed in [ref] , in more details in [ref] , and were recently addressed also in [ref] .
Bounds on Neutron- Mirror Neutron Mixing from Pulsar Timings and Gravitational Wave Detections · Introduction · 0.88
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were briefly discussed in [ref] , in more details in [ref] , and were recently addressed also in [ref] .
Constraining Mirror Dark Matter Inside Neutron Stars · Introduction · 0.88
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The neutron star conversion into dark neutron star via the transitional magnetic moment induced by the neutron–dark neutron mixing was discussed in Refs. [ref] .
Neutron stars exclude light dark baryons · Conclusions · 0.94
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