AI 中文总结
研究短伽马射线暴磁星场与初始自旋周期关系，通过分析33个Swift sGRBs推导相关数据，首次得出其与长伽马射线暴一致的幂律$B_p$-$P_0$相关性，完善统计并统一磁星物理，提供观测约束。
AI 中文摘要
$B_p$-$P_0$相关性是磁星引擎物理的关键探测手段。虽然这种标度关系在长伽马射线暴（lGRBs）中已被牢固确立，但对短伽马射线暴（sGRBs）的系统研究仍未开展，这使得两者之间的物理差异难以界定。本文分析了33个显示出新生毫秒磁星自旋下降导致显著X射线平台的Swift sGRBs，推导了它们的初始自旋周期$P_0$和极向磁场$B_p$。sGRB磁星的$P_0$范围为$[1.73,18.28]\ \mathrm{ms}$，$B_p$范围为$[0.06,2.82]\times10^{17}\ \mathrm{G}$（$\langle B_p\rangle = 7.05\times10^{16}\ \mathrm{G}$），比lGRB磁星（$B_p\in[0.39,23.08]\times10^{15}\ \mathrm{G}$；$\langle B_p\rangle = 3.69\times10^{15}\ \mathrm{G}$）磁化程度高得多。首次推导了GRBs一致的幂律$B_p$-$P_0$相关性：sGRBs的标度为$\log B_p=(0.84\pm0.07)\log P_0+(15.79\pm0.07)$，其斜率与lGRBs的高度一致，$\log B_p=(0.83\pm0.09)\log P_0+(14.92\pm0.06)$。相近的斜率意味着通用的磁星自旋下降机制，而截距之间的垂直偏移则表明前身星通道不同。这种标度关系为区分GRB的形成途径提供了新的诊断方法。在标准自旋加速模型框架内，sGRBs的质量吸积率（$\dot{M}\sim1\times10^{-1}$至$3\times10^{-1}\,M_\odot\,\mathrm{s}^{-1}$）显著高于lGRBs（$\dot{M}\sim10^{-4}$至$1\times10^{-1}\,M_\odot\,\mathrm{s}^{-1}$）。我们的工作完善了sGRBs缺失的$B_p$-$P_0$统计，定量统一了它们与lGRBs的磁星物理，并为相对论瞬变的起源多样性提供了新的观测约束。
英文摘要
The $B_p$--$P_0$ correlation serves as a critical probe of magnetar engine physics. Although this scaling relation has been firmly established for long gamma-ray bursts (lGRBs), systematic investigations for short GRBs (sGRBs) remain absent, leaving the physical differences between the two populations poorly constrained. Here we analyze 33 Swift sGRBs exhibiting prominent X-ray plateaus from newborn millisecond magnetar spin-down, and derive their initial spin period $P_0$ and polar magnetic field $B_p$. sGRB magnetars span $P_0 \in [1.73,\,18.28]\ \mathrm{ms}$ and $B_p \in [0.06,\,2.82] \times 10^{17}\ \mathrm{G}$ ($\langle B_p \rangle = 7.05 \times 10^{16}\ \mathrm{G}$), significantly more magnetized than lGRB magnetars ($B_p \in [0.39,\,23.08] \times 10^{15}\ \mathrm{G}$; $\langle B_p \rangle = 3.69 \times 10^{15}\ \mathrm{G}$). For the first time, we derive consistent power-law $B_p$--$P_0$ correlations for GRBs : the scaling for sGRBs is $\log B_p = (0.84\pm0.07)\log P_0 + (15.79\pm0.07)$, whose slope is highly consistent with that of lGRBs, $\log B_p = (0.83\pm0.09)\log P_0 + (14.92\pm0.06)$. The near-identical slopes imply a universal magnetar spin-down mechanism, while the vertical offset between intercepts traces divergent progenitor channels. This scaling relation thus offers a new diagnostic to disentangle the formation pathways of GRB. Within the framework of the standard spin-up model, the mass accretion rates of sGRBs ($\dot{M} \sim 1 \times 10^{-1}$ to $3 \times 10^{-1}\,M_\odot\,\mathrm{s}^{-1}$) are substantially higher than those of lGRBs ($\dot{M} \sim 10^{-4}$ to $1 \times 10^{-1}\,M_\odot\,\mathrm{s}^{-1}$). Our work completes the missing $B_p$--$P_0$ statistics for sGRBs, quantitatively unifies their magnetar physics with lGRBs, and provides new observational constraints on the origin diversity of relativistic transients.
Comments10 pages, 2 figures and 1 table
