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Hybrid stars may have an inverted structure
High Energy Astrophysical Phenomena · Submitted 22 Nov 2022
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that the interplay between the hadronic matter and quark matter compositions of cross stars can help to reconcile the small radii constraints indicated by the LIGO/Virgo GW170817 event, the large radii constraints set for massive compact stars by recent NICER X-ray observations, and the recent observation of the most-massive pulsar PSR J0952-0607.
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The abstract, sentence by sentence
We propose a new stellar structure of compact stars, the ``cross stars" that consist of a hadronic matter core and a quark matter crust, with an inverted structure compared to the conventional hybrid stars. This distinct stellar structure naturally arises from the quark matter to hadronic matter transition associated with the chemical potential crossing, in the context of the quark matter hypothesis that either strange or up-down quark matter is the ground state of baryonic matter at low pressure. We find that the interplay between the hadronic matter and quark matter compositions of cross stars can help to reconcile the small radii constraints indicated by the LIGO/Virgo GW170817 event, the large radii constraints set for massive compact stars by recent NICER X-ray observations, and the recent observation of the most-massive pulsar PSR J0952-0607. This leaves more space open for the equation of states of both hadronic matter and quark matter.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We propose a new stellar structure of compact stars, the ``cross stars" that consist of a hadronic matter core and a quark matter crust, with an inverted structure compared to the conventional hybrid stars. | contribution 1.00 | 0.80 | 0.67 | speculative 0.49 |
| s1 | This distinct stellar structure naturally arises from the quark matter to hadronic matter transition associated with the chemical potential crossing, in the context of the quark matter hypothesis that either strange or up-down quark matter is the ground state of baryonic matter at low pressure. | interpretation 0.45 | 0.28 | 0.09 | asserted 0.98 |
| s2 | We find that the interplay between the hadronic matter and quark matter compositions of cross stars can help to reconcile the small radii constraints indicated by the LIGO/Virgo GW170817 event, the large radii constraints set for massive compact stars by recent NICER X-ray observations, and the recent observation of the most-massive pulsar PSR J0952-0607. | result 0.95 | 0.93 | 0.30 | asserted 0.87 |
| s3 | This leaves more space open for the equation of states of both hadronic matter and quark matter. | interpretation 0.97 | 0.50 | 0.09 | asserted 0.80 |
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The paper
Original abstract
We propose a new stellar structure of compact stars, the ``cross stars" that consist of a hadronic matter core and a quark matter crust, with an inverted structure compared to the conventional hybrid stars. This distinct stellar structure naturally arises from the quark matter to hadronic matter transition associated with the chemical potential crossing, in the context of the quark matter hypothesis that either strange or up-down quark matter is the ground state of baryonic matter at low pressure. We find that the interplay between the hadronic matter and quark matter compositions of cross stars can help to reconcile the small radii constraints indicated by the LIGO/Virgo GW170817 event, the large radii constraints set for massive compact stars by recent NICER X-ray observations, and the recent observation of the most-massive pulsar PSR J0952-0607. This leaves more space open for the equation of states of both hadronic matter and quark matter.
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References
How the literature uses it
5 arXiv papers cite this in 9 sentences
Papers citing it · 5 sentences without a confident label
Uses its data or values 1 paper
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Referring to Ref. [ref] , we choose a typical benchmark set $B=(20, 35, 50) MeV/fm^3≈( 111^4, 128^4, 140^4) MeV^4$ for both $ud$QM and SQM.
Radial and Non-Radial Oscillations of Inverted Hybrid Stars · A Recap on the EOS and $M$-$R$ Relation · 0.84
Compares with it 1 paper
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Note that this study also differs from our previous study of self-bound hybrid-star scenarios [ref] that were based on unconventional phase transitions [ref] inside self-bound compact stars [ref] composed of quark matter [ref] or quark-cluster matter [ref] , where the small-radius behavior at low mass that benefits accommodating HESS J1731–347 is aided by the finite-density self-bound star surface.
Can a slow and strong phase transition in neutron stars relieve major compact-star observation tensions? · Introduction · 0.87
Cites it as background 2 papers
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Quark matter, a state comprised of deconfined free-flowing quarks, can possibly exist inside the neutron star core (i.e. hybrid stars [ref] ) or the crust (i.e. inverted hybrid stars [ref] ), or constitutes entire star called quark star.
Rescaling strange-cluster stars and its implications on gravitational-wave echoes · Introduction · 0.96
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If they are stable at zero pressure, either in form of strange quark matter (SQM) [ref] or up-down quark matter ($ud$QM) [ref] , they can constitute an entire quark star [ref] or the crust (i.e. inverted hybrid stars [ref] ), both with potentially distinct astrophysical implications [ref] .
Hybrid Strangeon Stars · Introduction · 0.96
What it cites · 54 sentences without a confident label
Uses the method or tool of 5 papers
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For CrSs, the matching condition [ref] $y(r_d^+) - y(r_d^-) = -4πr_d^3 Δρ_d /(m(r_d)+4πr_d^3 P(r_d))$ should be imposed at $r_d$ (i.e., the hadronic core radius $r_cr$ and the CrS radius $R$), where an energy density jump $Δρ_d$ occurs.
Comment on "Tidal Love numbers of neutron and self-bound quark stars" · Astrophysical Implications · 0.88
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For CrSs, the matching condition [ref] $y(r_d^+) - y(r_d^-) = -4πr_d^3 Δρ_d /(m(r_d)+4πr_d^3 P(r_d))$ should be imposed at $r_d$ (i.e., the hadronic core radius $r_cr$ and the CrS radius $R$), where an energy density jump $Δρ_d$ occurs.
Relativistic tidal properties of neutron stars · Astrophysical Implications · 0.88
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To compare with gravitational wave observations, we can further compute the dimensionless tidal deformability $Λ=2k_2/(3C^5)$, where $C=M/R$ is the compactness and $k_2$ is the Love number that characterizes the stars' response to external disturbances [ref] .
Tidal deformability of neutron stars with realistic equations of state and their gravitational wave signatures in binary inspiral · Astrophysical Implications · 0.92
Uses data or values from 3 papers
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More explicitly, the depicted maximum masses of CrSs all meet the two solar mass constraints from pulsar mass measurements, in particular, $2.01^+0.17_-0.11 M_⊙$ for J0348+0432 [ref] , $2.14^+0.20_-0.18 M_⊙$ for J0740+6620 [ref] and $2.35^+0.17_-0.17 M_⊙$ for PSR J0952-0607 [ref] .
A Massive Pulsar in a Compact Relativistic Binary · Astrophysical Implications · 0.84
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More explicitly, the depicted maximum masses of CrSs all meet the two solar mass constraints from pulsar mass measurements, in particular, $2.01^+0.17_-0.11 M_⊙$ for J0348+0432 [ref] , $2.14^+0.20_-0.18 M_⊙$ for J0740+6620 [ref] and $2.35^+0.17_-0.17 M_⊙$ for PSR J0952-0607 [ref] .
Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar · Astrophysical Implications · 0.84
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More explicitly, the depicted maximum masses of CrSs all meet the two solar mass constraints from pulsar mass measurements, in particular, $2.01^+0.17_-0.11 M_⊙$ for J0348+0432 [ref] , $2.14^+0.20_-0.18 M_⊙$ for J0740+6620 [ref] and $2.35^+0.17_-0.17 M_⊙$ for PSR J0952-0607 [ref] .
PSR J0952-0607: The Fastest and Heaviest Known Galactic Neutron Star · Astrophysical Implications · 0.84
Cites as background 28 papers
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Recent detections of gravitational wave (GW) signals from compact binary mergers by the LIGO/Virgo collaborations [ref] have greatly moved our understanding of black holes and compact stars forward.
GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2 · Introduction · 1.00
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Recent detections of gravitational wave (GW) signals from compact binary mergers by the LIGO/Virgo collaborations [ref] have greatly moved our understanding of black holes and compact stars forward.
Properties of the binary neutron star merger GW170817 · Introduction · 1.00
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Recent detections of gravitational wave (GW) signals from compact binary mergers by the LIGO/Virgo collaborations [ref] have greatly moved our understanding of black holes and compact stars forward.
GW170817: Measurements of Neutron Star Radii and Equation of State · Introduction · 1.00
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