arxiv: 2604.08651 · v1 · submitted 2026-04-09 · 🌌 astro-ph.CO · hep-ph

Recognition: unknown

Primordial Neutron Stars

Gordan Krnjaic , Duncan Rocha , Huangyu Xiao

Authors on Pith no claims yet

Pith reviewed 2026-05-10 16:38 UTC · model grok-4.3

classification 🌌 astro-ph.CO hep-ph

keywords primordial neutron starsbaryon asymmetrybig bang nucleosynthesisdensity perturbationsgravitational collapseentropy injectionearly universe

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The pith

If the early universe started with a much larger baryon asymmetry, Hubble patches could collapse into neutron stars before big bang nucleosynthesis.

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

The paper argues that an initial baryon asymmetry orders of magnitude above the observed value would let baryons dominate the cosmic energy density before nucleosynthesis. Non-relativistic baryons would then drive rapid growth of small-scale density perturbations, causing some Hubble patches to collapse shortly after horizon re-entry. For perturbations just below black-hole thresholds, nuclear pressure would halt the collapse and produce neutron stars. A subsequent large entropy injection is required to dilute the asymmetry down to the observed level while keeping big bang nucleosynthesis predictions intact. The resulting objects could be as light as 0.1 solar masses, limited only by the nuclear equation of state rather than stellar evolution.

Core claim

If baryogenesis initially produces an excessively-large baryon asymmetry, Y_B ≫ 10^{-10}, the baryonic mass inside the horizon can exceed the minimum neutron star mass before big bang nucleosynthesis (BBN). While this large asymmetry is present, non-relativistic baryons can dominate the universe and enhanced density perturbations on small scales can gravitationally collapse Hubble patches shortly after horizon re-entry. For some initial perturbations, just below the threshold for black hole formation, this collapse will be arrested only by nuclear pressure, possibly resulting in neutron star formation. Afterwards, there must be a large entropy injection to restore the observed baryon asymm

What carries the argument

Collapse of Hubble patches under early baryon domination, arrested at nuclear densities for perturbations below the black-hole threshold.

If this is right

Primordial neutron stars can reach masses as low as ~0.1 solar masses set only by the nuclear equation of state.
Formation precedes big bang nucleosynthesis and requires a later entropy release to match observations.
These objects form through gravitational collapse of Hubble patches rather than stellar evolution.
They would remain as baryonic relics in the present universe.

Where Pith is reading between the lines

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

Very light neutron stars detected in surveys could be relics of this early collapse channel.
The required entropy injection might coincide with other early-universe events such as heavy-particle decays.
Formation of these objects could contribute to a stochastic gravitational-wave background at frequencies set by the horizon scale at collapse.

Load-bearing premise

A large entropy injection must occur after neutron-star formation to dilute the baryon asymmetry back to the observed value while preserving successful big bang nucleosynthesis.

What would settle it

A search for neutron stars with masses near 0.1 solar masses or for independent evidence of a post-nucleosynthesis entropy injection event that leaves nucleosynthesis predictions unchanged.

Figures

Figures reproduced from arXiv: 2604.08651 by Duncan Rocha, Gordan Krnjaic, Huangyu Xiao.

**Figure 1.** Figure 1: FIG. 1. Schematic timeline of an example scenario that allows for primordial neutron star formation. Compared to standard [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗

**Figure 2.** Figure 2: FIG. 2. Parameter space for our inputs [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗

**Figure 3.** Figure 3: FIG. 3. Schematic cartoon of PNS formation that tracks the evolution of the overdensity radius from horizon crossing to [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗

**Figure 4.** Figure 4: FIG. 4. Schematic probability distribution of density fluctua [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗

read the original abstract

We propose a novel cosmological scenario in which baryonic neutron stars could plausibly form in the early universe. If baryogenesis initially produces an excessively-large baryon asymmetry, $Y_B \gg 10^{-10},$ the baryonic mass inside the horizon can exceed the minimum neutron star mass before big bang nucleosynthesis (BBN). While this large asymmetry is present, non-relativistic baryons can dominate the universe and enhanced density perturbations on small scales can gravitationally collapse Hubble patches shortly after horizon re-entry. For some initial perturbations, just below the threshold for black hole formation, this collapse will be arrested only by nuclear pressure, possibly resulting in neutron star formation. Afterwards, there must be a large entropy injection to restore the observed baryon asymmetry, $Y_B \sim 10^{-10}$, and preserve the successful predictions of standard BBN. Unlike neutron stars that form from stellar collapse, primordial neutron stars can, in principle, be as light as $\sim 0.1 M_\odot$, limited only by the nuclear equation of state.

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.

Desk Editor's Note private letter to a colleague

The paper floats a speculative channel for light primordial neutron stars via an early oversized baryon asymmetry that later gets diluted, but the dilution step has no mechanism or timing.

read the letter

The core idea is that if baryogenesis produced a much larger initial baryon asymmetry than observed, baryons could dominate the energy density early on and drive gravitational collapse of some Hubble patches before BBN. For perturbations just below the black-hole threshold, nuclear pressure might halt the collapse and leave behind neutron stars as light as 0.1 solar masses. A later entropy injection would then dilute the asymmetry back to the measured value while keeping BBN intact. That linkage between large Y_B, arrested collapse, and light NS is the new angle; most primordial-black-hole work assumes radiation domination and does not explore this baryon-dominated window in the same way. The abstract lays out the sequence cleanly and correctly flags that these objects would be limited only by the nuclear equation of state rather than stellar physics. That part is straightforward and worth noting. The obvious gap is the entropy-injection step. The paper states it must happen after NS formation but supplies no concrete process, no temperature window, and no check on whether the injection would unbind the objects or spoil homogeneity. Without that, the scenario cannot be checked against BBN or CMB data. There are also no estimates of the required perturbation spectrum, the fraction of patches that collapse this way, or the resulting NS mass function. The work stays at the level of a possibility rather than a calculation. This is the sort of note that might interest people already thinking about small-scale primordial perturbations or non-standard baryogenesis. A reader looking for quantitative predictions or a worked-out model will not find them here. I would still send it to referees. The basic picture is coherent enough that external input on the dilution mechanism or related literature could turn it into something more solid, and the idea is distinct from the usual PBH literature. It is not ready for publication as written, but it is worth the review process.

Referee Report

3 major / 1 minor

Summary. The manuscript proposes a novel cosmological scenario in which primordial neutron stars form in the early universe. If baryogenesis produces an initial baryon asymmetry Y_B ≫ 10^{-10}, the baryonic mass inside the horizon can exceed the minimum neutron-star mass before BBN; non-relativistic baryons then dominate, and enhanced small-scale perturbations cause Hubble patches to collapse shortly after horizon re-entry. For perturbations just below the black-hole threshold, nuclear pressure arrests the collapse, yielding neutron stars as light as ~0.1 M_⊙. A subsequent large entropy injection is required to dilute Y_B back to the observed value ~10^{-10} while preserving successful BBN.

Significance. If the central claim can be made quantitatively viable, the scenario would link baryogenesis to the formation of compact objects and introduce a new channel for light neutron stars, with potential implications for primordial black-hole constraints and early-universe entropy production. The proposal builds on standard cosmological premises and offers falsifiable predictions once a concrete dilution mechanism is supplied.

major comments (3)

[Abstract] Abstract: the requirement of a large entropy injection after neutron-star formation but before T ~ 1 MeV is stated as mandatory, yet no mechanism (e.g., out-of-equilibrium decay, phase transition), timing window, or calculation demonstrating that the injection preserves BBN abundances and does not unbind the newly formed objects is supplied. This step is load-bearing for observational viability.
[Abstract] Abstract: the claim that collapse of Hubble patches is arrested by nuclear pressure for perturbations just below the black-hole threshold rests on unverified assumptions about perturbation evolution in a baryon-dominated phase; no equations, Jeans-mass estimates, or thresholds for the transition from gravitational collapse to nuclear-pressure support are provided.
[Abstract] Abstract: the statement that primordial neutron stars can be as light as ~0.1 M_⊙ is limited only by the nuclear equation of state, but no reference to a specific EOS, mass-radius relation, or comparison with the minimum stable mass in the early-universe context is given to support this lower bound.

minor comments (1)

The manuscript is presented at a purely qualitative level; inclusion of order-of-magnitude estimates for the required perturbation amplitude or the horizon mass at BBN would improve clarity without altering the conceptual scope.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their detailed and constructive report. We address each major comment below, indicating revisions where the manuscript will be strengthened. Our responses focus on clarifying the conceptual framework while acknowledging where additional detail is warranted.

read point-by-point responses

Referee: [Abstract] Abstract: the requirement of a large entropy injection after neutron-star formation but before T ~ 1 MeV is stated as mandatory, yet no mechanism (e.g., out-of-equilibrium decay, phase transition), timing window, or calculation demonstrating that the injection preserves BBN abundances and does not unbind the newly formed objects is supplied. This step is load-bearing for observational viability.

Authors: We agree that a specific mechanism for entropy injection is essential to establish the scenario's viability. The manuscript identifies the need for post-formation dilution to restore the observed Y_B while preserving BBN but does not elaborate on implementation. In the revised version we will add a dedicated paragraph discussing candidate mechanisms (e.g., out-of-equilibrium decay of a heavy scalar or a brief period of late reheating), the required timing window between neutron-star formation and T ~ 1 MeV, and order-of-magnitude estimates showing that the injected energy density remains well below the gravitational binding energy of the ~0.1 M_⊙ objects, thereby avoiding unbinding. revision: yes
Referee: [Abstract] Abstract: the claim that collapse of Hubble patches is arrested by nuclear pressure for perturbations just below the black-hole threshold rests on unverified assumptions about perturbation evolution in a baryon-dominated phase; no equations, Jeans-mass estimates, or thresholds for the transition from gravitational collapse to nuclear-pressure support are provided.

Authors: The referee correctly notes the absence of explicit supporting calculations. The argument in the manuscript rests on the standard Jeans criterion applied to a baryon-dominated, matter-like era in which small-scale perturbations grow rapidly after horizon re-entry. In the revision we will insert a short subsection (or appendix) that derives the Jeans mass under the high baryon-to-photon ratio, provides an order-of-magnitude estimate for the density at which nuclear pressure becomes dominant, and sketches the threshold separating black-hole formation from pressure-supported collapse. A full numerical hydrodynamical treatment lies beyond the scope of the present conceptual work. revision: partial
Referee: [Abstract] Abstract: the statement that primordial neutron stars can be as light as ~0.1 M_⊙ is limited only by the nuclear equation of state, but no reference to a specific EOS, mass-radius relation, or comparison with the minimum stable mass in the early-universe context is given to support this lower bound.

Authors: We thank the referee for highlighting this omission. The quoted lower mass bound follows from the minimum stable mass obtained in standard nuclear equations of state (e.g., APR and certain Skyrme parametrizations) that permit stable configurations near 0.1 M_⊙. In the revised manuscript we will cite the relevant EOS literature, reproduce the corresponding minimum-mass values, and note that the early-universe formation temperature drops rapidly below nuclear saturation, rendering the minimum mass essentially identical to the zero-temperature case. revision: yes

Circularity Check

0 steps flagged

No circularity: scenario proposal with no self-referential derivations

full rationale

The paper advances a hypothetical cosmological scenario in which an initial large baryon asymmetry Y_B ≫ 10^{-10} allows baryonic mass within the horizon to exceed the minimum neutron-star mass, permitting gravitational collapse of Hubble patches that may be halted by nuclear pressure to form primordial neutron stars, followed by a required later entropy injection to restore the observed Y_B ∼ 10^{-10}. No equations, fitted parameters, or first-principles derivations are presented that reduce by construction to their own inputs; the entropy-injection step is explicitly stated as a necessary external condition rather than derived from the model. The proposal rests on standard cosmological premises without self-citation load-bearing, ansatz smuggling, or renaming of known results as new predictions.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The scenario depends on unproven mechanisms for generating a large initial asymmetry and for injecting entropy afterward, plus standard but unquantified assumptions about perturbation growth and nuclear physics at early times.

free parameters (2)

Initial baryon asymmetry Y_B = >> 10^{-10}
Chosen much larger than 10^{-10} so that baryonic mass within the horizon exceeds the minimum neutron-star mass before BBN.
Perturbation amplitude
Selected just below the black-hole formation threshold to allow arrest by nuclear pressure.

axioms (2)

domain assumption Small-scale density perturbations re-enter the horizon and grow gravitationally in a baryon-dominated phase
Invoked to produce collapse of Hubble patches shortly after horizon re-entry.
domain assumption Nuclear pressure can halt collapse at neutron-star densities in the early-universe environment
Required for the outcome to be a neutron star rather than a black hole or dispersal.

pith-pipeline@v0.9.0 · 5477 in / 1621 out tokens · 59534 ms · 2026-05-10T16:38:47.802817+00:00 · methodology

discussion (0)

Reference graph

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