# Stripping Model for Short GRBs: The Impact of Nuclear Data

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## Abstract

**:**

## 1. Introduction

## 2. The Influence of the NS EoS on the Stripping Time ${\mathit{t}}_{\mathrm{str}}$

#### 2.1. The NS Inspiral Stage

#### 2.2. The Stable Mass Transfer Stage

#### 2.3. The NS EoS in the Low-Mass Region

#### 2.4. The Nuclear Parameters and the Stripping Time

## 3. r-Process during the LMNS Explosion

#### 3.1. On the Influence of the EoS on the Results of Nucleosynthesis

#### 3.2. Nucleosynthesis in the Inner Crust

#### 3.3. The Influence of Beta Decay Rates

## 4. Discussion and Conclusions

## Author Contributions

## Funding

## Data Availability Statement

## Conflicts of Interest

## Abbreviations

GRB | Gamma-ray burst |

GW | Gravitational wave |

NS | Neutron star |

LMNS | Low-mass NS |

BH | Black hole |

EoS | Equation of state |

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**Figure 1.**Structure of NSs with different masses. The lower wide panel corresponds to the minimum NS mass. The regions of the core, inner, and outer crusts are identified. See text for details.

**Figure 3.**The top and bottom panels show the dependence of the stripping time ${t}_{\mathrm{str}}$ and the LMNS mass ${M}_{\mathrm{us}}$, at which the mass-transfer stability is lost, on the parameter $\eta $. Crosses indicate calculations for the BSk EoS. See text for details.

**Figure 4.**Constraints on the parameters of the nuclear EoS obtained from the PREX-II experiment and the combined astrophysical observations. The black line corresponds to the upper bound obtained from comparing the calculated stripping time with the GW170817-GRB170817A time delay. See the text for details.

**Figure 5.**Limitations of the symmetry energy slope parameter from various experiments and astrophysical observations. See text for details.

**Figure 6.**Integral curve $Y\left(A\right)$ of the results of nucleosynthesis in the outer crust using the BSk22 (curve 2, blue) and BSk25 (curve 1, red). The layers of the outer crust are taken into account, starting from No. 9 (see Table 1), having a total mass of $M\sim $0.0025${M}_{\odot}$. Solar abundance is shown by dots.

**Figure 7.**Composition of the inner crust for BSk25 as a function of the Lagrangian variable (mass) m. The corresponding density values are given on the upper axis. See text for details.

**Figure 8.**$N-Z$ chart of nuclei included in our calculations. The position of the neutron-rich cluster is indicated by a green asterisk. The arrows indicate the direction of dissociation of this cluster in two limiting cases.

**Figure 9.**The result of nucleosynthesis $Y\left(A\right)$ depending on the limit decompression options: only evaporation of neutrons $(\gamma ,n)$ (curve 1, blue) or only beta decays ${\beta}^{-}$ (curve 2, red). Dots are the solar abundance.

**Figure 10.**Dependence of the abundance of heavy nuclei for the outer layer of the inner crust when using different beta decay rates in the calculations: curve 1 (green) is for beta decay rates obtained from the drop model (FRDM) [59], and curve 2 (red) is based on the finite amplitude method (FAM) [56].

№ ${}^{*}$ | Composition | ${\mathit{T}}_{9}^{\mathbf{max}}\left(\mathit{t}\right)$ | $lg{\mathit{\rho}}^{\mathbf{max}}\left(\mathit{t}\right)$ | ${\mathit{Y}}_{\mathbf{e}}$ | $\mathit{\Delta}\mathit{M},{10}^{-4}{\mathit{M}}_{\odot}$ | $\sum \mathit{M},{10}^{-4}{\mathit{M}}_{\odot}$ | ||||||
---|---|---|---|---|---|---|---|---|---|---|---|---|

BSk22 | BSk25 | BSk22 | BSk25 | BSk22 | BSk25 | BSk22 | BSk25 | BSk22 | BSk25 | BSk22 | BSk25 | |

18 | ${}^{128}$Sr | - | 0.98 | - | 11.64 | - | 0.297 | - | 0.88 | - | 0.88 | - |

17 | ${}^{126}$Sr | - | 1.19 | - | 11.60 | - | 0.302 | - | 1.25 | - | 2.13 | - |

16 | ${}^{124}$Sr | - | 1.39 | - | 11.56 | - | 0.306 | - | 0.80 | - | 2.93 | - |

15 | ${}^{122}$Sr | ${}^{122}$Sr | 1.62 | 8.63 | 11.49 | 11.59 | 0.311 | 0.311 | 3.60 | 2.64 | 6.53 | 2.64 |

14 | ${}^{121}$Y | ${}^{120}$Sr | 1.96 | 10.01 | 11.38 | 11.52 | 0.322 | 0.317 | 1.60 | 1.90 | 8.13 | 4.54 |

13 | ${}^{122}$Zr | ${}^{121}$Y | 2.17 | - | 11.31 | - | 0.328 | 0.322 | 1.48 | 1.10 | 9.61 | 5.64 |

12 | ${}^{124}$Mo | ${}^{122}$Zr | 2.59 | 10.57 | 11.20 | 11.39 | 0.339 | 0.328 | 3.87 | 2.20 | 13.48 | 7.84 |

11 | ${}^{80}$Ni | ${}^{124}$Mo | 3.19 | 11.44 | 11.01 | 11.24 | 0.350 | 0.339 | 4.95 | 4.10 | 18.43 | 11.94 |

10 | ${}^{78}$Ni | ${}^{126}$Ru | 3.80 | - | 10.84 | - | 0.359 | 0.349 | 1.74 | 1.05 | 20.17 | 12.99 |

9 | ${}^{76}$Ni | ${}^{78}$Ni | 4.27 | 13.76 | 10.74 | 10.88 | 0.368 | 0.359 | 4.92 | 7.00 | 25.09 | 19.99 |

8 | - | ${}^{80}$Zn | - | 14.74 | - | 10.58 | - | 0.375 | - | 5.10 | - | 25.09 |

Model | Before Decompression | After Decompression | |||||||
---|---|---|---|---|---|---|---|---|---|

$\mathit{Z}$ | $\mathit{A}$ | ${\mathit{N}}_{\mathrm{free}}$ | Evaporated n | ${\mathit{Z}}_{\mathrm{seed}}$ | ${\mathit{A}}_{\mathrm{seed}}$ | ${\mathit{Y}}_{\mathrm{seed}}$ | ${\mathit{Y}}_{\mathrm{n}}$ | ${\mathit{Y}}_{\mathrm{e}}$ | |

$(\gamma ,n)$ | 50 | 174 | 186 | 22 | 50 | 152 | 0.00278 | 0.578 | 0.139 |

${\beta}^{-}$ | 50 | 174 | 186 | 0 | 54 | 174 | 0.00278 | 0.517 | 0.150 |

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**MDPI and ACS Style**

Yudin, A.; Kramarev, N.; Panov, I.; Ignatovskiy, A.
Stripping Model for Short GRBs: The Impact of Nuclear Data. *Particles* **2023**, *6*, 784-800.
https://doi.org/10.3390/particles6030050

**AMA Style**

Yudin A, Kramarev N, Panov I, Ignatovskiy A.
Stripping Model for Short GRBs: The Impact of Nuclear Data. *Particles*. 2023; 6(3):784-800.
https://doi.org/10.3390/particles6030050

**Chicago/Turabian Style**

Yudin, Andrey, Nikita Kramarev, Igor Panov, and Anton Ignatovskiy.
2023. "Stripping Model for Short GRBs: The Impact of Nuclear Data" *Particles* 6, no. 3: 784-800.
https://doi.org/10.3390/particles6030050