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arxiv: 2606.02681 · v1 · pith:WPAOWJHSnew · submitted 2026-06-01 · 🌀 gr-qc

Quark Stars in Ricci-Determinant Gravity with an Interacting Quark Equation of State

Loreany F. Ara\'ujo , Krishna Pada Das This is my paper

Pith reviewed 2026-06-28 13:10 UTC · model grok-4.3

classification 🌀 gr-qc
keywords quark starsRicci-determinant gravityinteracting quark equation of statemass-radius relationcompactnessstellar stabilitymodified gravity
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The pith

Quark stars become less compact in Ricci-determinant gravity than in general relativity.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper studies static spherically symmetric quark stars with an interacting quark equation of state inside Ricci-Determinant gravity. It adopts the relativistic stellar structure equations from the literature and compares the resulting mass-radius relations and stability criteria to general relativity. The model produces lower compactness for quark stars, the opposite of what occurs for hadronic stars. Compactness depends on gravitational binding energy in a manner that breaks the usual universality. Objects with high central densities are forbidden once perturbative terms grow larger than roughly half the ordinary GR contribution, because instability sets in.

Core claim

In Ricci-Determinant gravity with an interacting quark equation of state, the model predicts a reduction in the compactness of quark stars. This parameter is also sensitive to gravitational binding-energy analysis, revealing a breakdown of the assumed universality. Furthermore, the formation of objects with high central densities is restricted by the instability conditions that arise when the contribution of perturbative terms exceeds by approximately half the contribution of ordinary GR.

What carries the argument

Relativistic stellar structure equations adapted to Ricci-Determinant gravity that incorporate perturbative corrections to the Einstein equations.

If this is right

  • Quark-star compactness decreases relative to general relativity for the same central density.
  • Gravitational binding-energy relations lose their universality for quark stars.
  • Stable configurations cannot reach the high central densities allowed in general relativity once perturbative terms exceed roughly half the GR contribution.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The contrast with hadronic stars indicates that the reduction in compactness depends on the specific equation of state.
  • The same perturbative threshold may impose density limits on other compact objects modeled in this gravity theory.

Load-bearing premise

The relativistic stellar structure equations for compact objects derived in the literature apply directly and without modification to the Ricci-Determinant gravity theory when solving for quark-star configurations.

What would settle it

Discovery of a stable quark star whose compactness is not reduced relative to general relativity, or whose central density exceeds the threshold where perturbative terms reach half the GR contribution, would falsify the predicted reduction and instability limit.

Figures

Figures reproduced from arXiv: 2606.02681 by Krishna Pada Das, Loreany F. Ara\'ujo.

Figure 1
Figure 1. Figure 1: FIG. 1. Interacting quark matter EOS [Eq. ( [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Mass–radius relations in the Ricci-determinant model governed by the geometrically effective parameter [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Mass and radius deviations from general relativity in the Ricci-determinant model for different values of [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Total mass in Ricci-determinant gravity for stability [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Relative contribution of the Ricci-determinant gravity corrections with respect to GR ( [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Mass-compactness relations for objects with different [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. Analysis of the gravitational binding energy in RD gravity. Panel (a) shows its dependence on the central density, while [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
read the original abstract

In the present study, we explore the fundamental properties of static, spherically symmetric quark stars composed of quark matter with an interacting quark equation of state (EoS) within the framework of Ricci-Determinant gravity. To this end, we adopt the relativistic stellar structure equations for compact objects derived in the literature. Our primary objective is to investigate deviations from General Relativity (GR) in key physical characteristics, particularly the mass--radius relation and stability criteria, arising from the free parameters of this extended gravitational theory. We see that, unlike the hadronic case, the model predicts a reduction in the compactness of quark stars. This parameter is also sensitive to gravitational binding-energy analysis, revealing a breakdown of the assumed universality. Furthermore, the formation of objects with high central densities is restricted by the instability conditions that arise when the contribution of perturbative terms exceeds by approximately half the contribution of ordinary GR, indicating a clear limitation in the theory.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The manuscript investigates static, spherically symmetric quark stars with an interacting quark equation of state in Ricci-Determinant gravity. It adopts the relativistic stellar structure equations from the literature to compute mass-radius relations and stability criteria, reporting a reduction in compactness (unlike the hadronic case), sensitivity of compactness to gravitational binding-energy analysis with breakdown of universality, and an instability restricting high central densities when perturbative terms exceed approximately half the GR contribution.

Significance. If the structure equations are valid under the modified action, the work could constrain the free parameters of Ricci-Determinant gravity via compact-object observations and demonstrate qualitative differences from GR for quark stars.

major comments (2)
  1. [Abstract and stellar structure section] Abstract and the section adopting the stellar structure equations: the hydrostatic equilibrium condition is taken directly from the GR literature without re-derivation from the Ricci-Determinant field equations. In a modified-gravity theory the generalized TOV equation must be obtained from the new metric variation; all reported results on compactness reduction, binding-energy universality breakdown, and the ~half-GR instability threshold rest on this unverified assumption.
  2. [Abstract and results section] The quantitative claim that instability arises 'when the contribution of perturbative terms exceeds by approximately half the contribution of ordinary GR' is stated without an explicit equation defining the ratio or the threshold; this renders the reported limitation on high central densities non-reproducible from the given text.
minor comments (1)
  1. [Abstract] The phrasing 'we see that' in the abstract is informal for a journal manuscript.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed review and valuable comments on our manuscript. We address the major comments point by point below.

read point-by-point responses

  1. Referee: [Abstract and stellar structure section] Abstract and the section adopting the stellar structure equations: the hydrostatic equilibrium condition is taken directly from the GR literature without re-derivation from the Ricci-Determinant field equations. In a modified-gravity theory the generalized TOV equation must be obtained from the new metric variation; all reported results on compactness reduction, binding-energy universality breakdown, and the ~half-GR instability threshold rest on this unverified assumption.

    Authors: The manuscript explicitly states that the relativistic stellar structure equations are adopted from the literature where they were derived for Ricci-Determinant gravity. We will revise the relevant section to include explicit citations to the papers containing the derivation of the generalized TOV equation from the metric variation of the Ricci-Determinant action, making clear that the equations are not taken from the GR literature. revision: yes

  2. Referee: [Abstract and results section] The quantitative claim that instability arises 'when the contribution of perturbative terms exceeds by approximately half the contribution of ordinary GR' is stated without an explicit equation defining the ratio or the threshold; this renders the reported limitation on high central densities non-reproducible from the given text.

    Authors: We agree that an explicit definition of the ratio and threshold is needed for reproducibility. In the revised manuscript we will insert the precise mathematical definition of the ratio of perturbative gravity terms to the GR contribution together with the numerical threshold value at which the instability condition is applied. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper states it adopts the relativistic stellar structure equations from the literature and performs numerical integrations of mass-radius and stability relations using an interacting quark EoS plus free parameters of Ricci-Determinant gravity. The reported outcomes (reduced compactness relative to hadronic case, breakdown of binding-energy universality, instability when perturbative terms exceed ~half the GR contribution) are presented as results of those integrations rather than identities or fits forced by construction. No self-definitional steps, fitted inputs renamed as predictions, or self-citation chains that reduce the central claims to the inputs are exhibited in the quoted abstract or described structure. The derivation chain therefore retains independent numerical content.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claims rest on the direct applicability of literature-derived stellar structure equations to this modified gravity and on the validity of the chosen interacting quark EoS; no independent verification of either is supplied in the abstract.

free parameters (1)
  • free parameters of Ricci-Determinant gravity
    Deviations from GR and the reported compactness and stability limits depend on these parameters; no specific values or fitting procedure given in abstract.
axioms (1)
  • domain assumption relativistic stellar structure equations derived in the literature remain valid without modification in Ricci-Determinant gravity
    Paper states it adopts these equations directly.

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