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Combustion of a hadronic star into a quark star: the turbulent and the diffusive regimes
Nuclear Theory · Submitted 27 Jun 2015
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We argue that the full conversion of a hadronic star into a quark or a hybrid star occurs within two different regimes separated by a critical value of the density of the hadronic phase $\overline{n_h}$.
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The abstract, sentence by sentence
We argue that the full conversion of a hadronic star into a quark or a hybrid star occurs within two different regimes separated by a critical value of the density of the hadronic phase $\overline{n_h}$. The first stage, occurring for $n_h>\overline{n_h}$, is characterized by turbulent combustion and lasts typically a few ms. During this short time-scale neutrino cooling is basically inactive and the star heats up thanks to the heat released in the conversion. In the second stage, occurring for $n_h<\overline{n_h}$, turbulence is not active anymore, and the conversion proceeds on a much longer time scale (of the order of tens of seconds), with a velocity regulated by the diffusion and the production of strange quarks. At the same time, neutrino cooling is also active. The interplay between the heating of the star due to the slow conversion of its outer layers (with densities smaller than $\overline{n_h}$) and the neutrino cooling of the forming quark star leads to a quasi-plateau in the neutrino luminosity which, if observed, would possibly represent a unique signature for the existence of quark matter inside compact stars. We will discuss the phenomenological implications of this scenario in particular in connection with the time structure of long gamma-ray-bursts.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We argue that the full conversion of a hadronic star into a quark or a hybrid star occurs within two different regimes separated by a critical value of the density of the hadronic phase $\overline{n_h}$. | contribution 0.51 | 0.61 | 0.67 | asserted 0.46 |
| s1 | The first stage, occurring for $n_h>\overline{n_h}$, is characterized by turbulent combustion and lasts typically a few ms. | result 0.88 | 0.58 | 0.16 | asserted 0.99 |
| s2 | During this short time-scale neutrino cooling is basically inactive and the star heats up thanks to the heat released in the conversion. | result 0.93 | 0.46 | 0.05 | asserted 0.99 |
| s3 | In the second stage, occurring for $n_h<\overline{n_h}$, turbulence is not active anymore, and the conversion proceeds on a much longer time scale (of the order of tens of seconds), with a velocity regulated by the diffusion and the production of strange quarks. | result 0.85 | 0.57 | 0.17 | asserted 1.00 |
| s4 | At the same time, neutrino cooling is also active. | result 0.76 | 0.38 | 0.04 | asserted 1.00 |
| s5 | The interplay between the heating of the star due to the slow conversion of its outer layers (with densities smaller than $\overline{n_h}$) and the neutrino cooling of the forming quark star leads to a quasi-plateau in the neutrino luminosity which, if observed, would possibly represent a unique signature for the existence of quark matter inside compact stars. | interpretation 0.85 | 0.44 | 0.59 | hedged possibility 0.86 |
| s6 | We will discuss the phenomenological implications of this scenario in particular in connection with the time structure of long gamma-ray-bursts. | future work 0.52 | 0.43 | 0.06 | unclear 0.72 |
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The paper
Original abstract
We argue that the full conversion of a hadronic star into a quark or a hybrid star occurs within two different regimes separated by a critical value of the density of the hadronic phase $\overline{n_h}$. The first stage, occurring for $n_h>\overline{n_h}$, is characterized by turbulent combustion and lasts typically a few ms. During this short time-scale neutrino cooling is basically inactive and the star heats up thanks to the heat released in the conversion. In the second stage, occurring for $n_h<\overline{n_h}$, turbulence is not active anymore, and the conversion proceeds on a much longer time scale (of the order of tens of seconds), with a velocity regulated by the diffusion and the production of strange quarks. At the same time, neutrino cooling is also active. The interplay between the heating of the star due to the slow conversion of its outer layers (with densities smaller than $\overline{n_h}$) and the neutrino cooling of the forming quark star leads to a quasi-plateau in the neutrino luminosity which, if observed, would possibly represent a unique signature for the existence of quark matter inside compact stars. We will discuss the phenomenological implications of this scenario in particular in connection with the time structure of long gamma-ray-bursts.
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References
How the literature uses it
4 arXiv papers cite this in 5 sentences
Papers citing it · 3 sentences without a confident label
Cites it as support 1 paper
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This result was obtained in numerical simulations [ref] and has been confirmed and interpreted analytically in [ref] .
How to Test the Two-Families Scenario · Quark deconfinement · 0.96
Cites it as background 1 paper
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The properties of single quark stars have been studied by numerous works [ref] , while the study of the binary quark-star mergers have been explored far less [ref] .
Fully general-relativistic simulations of isolated and binary strange quark stars · Introduction · 0.98
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