论文标题
GRB170817A的中央发动机：基于多通电器量热法和事件时机的中子星与Kerr黑洞
Central engine of GRB170817A: Neutron star versus Kerr black hole based on multimessenger calorimetry and event timing
论文作者
论文摘要
The central engine of GRB170817A post-merger to GW170817 is probed by GW-calorimetry and event timing, applied to a post-merger descending chirp which can potentially break the degeneracy in spin-down of a neutron star or black hole remnant by the relatively large energy reservoir in the angular momentum, $E_J$, of the latter according to the Kerr metric.该分析源自模型 - 反应频谱图，对时间对称蝴蝶匹配的过滤产生的对上升和下降的呼叫具有相等的敏感性。通过软件注入实验产生的响应曲线对灵敏度进行了校准。 GRB170817A中央发动机的候选发射的统计显着性由虚假警报的概率（PFA； I型错误）表达，该概率从事件成像分析中得出。 PDF的启动时间$ t_s $是通过可用频谱图的高分辨率图像分析确定的。对于合并的（H1，L1） - LIGO探测器的光谱图，PFA $ P_1 $源自$ T_S $的因果关系，给定GW170817-GRB17081A。单个H1和L1分析中介绍了统计独立的确认，在其各自的$ T_S $的观察结果中，第二个PFA $ P_2 $一致性。自均值和时间（分别）定时差异以来，PFA的组合源自其产品，在统计上是独立的。适用于GW170817-GRB170817A，事件计时$ t_s $ producation $ p_1 = 8.3 \ times 10^{ - 4} $和$ p_2 = 4.9 \ times 10^{ - 5} $ fused $ {\ cal e} _ {gw} $ {gw} $ cime cime， （$ p_1p_2 = 4.1 \ times 10^{ - 8} $，等效$ z $ -score 5.48）。 $ {\ cal e} _ {gw} $超过了GW170817的直接后，超质量中子星的$ e_j $，但它与$ e_j $一致，$ e_j $是在延迟的重力倒塌中重新焕发的。通过产生黑洞的能量核心偏转超新星可能会预期类似的排放。 （abbr。）
The central engine of GRB170817A post-merger to GW170817 is probed by GW-calorimetry and event timing, applied to a post-merger descending chirp which can potentially break the degeneracy in spin-down of a neutron star or black hole remnant by the relatively large energy reservoir in the angular momentum, $E_J$, of the latter according to the Kerr metric. This analysis derives from model-agnostic spectrograms with equal sensitivity to ascending and descending chirps generated by time-symmetric butterfly matched filtering. The sensitivity was calibrated by response curves generated by software injection experiments. The statistical significance for candidate emission from the central engine of GRB170817A is expressed by probabilities of false alarm (PFA; type I errors) derived from an event-timing analysis. PDFs were derived for start-time $t_s$, identified via high-resolution image analyses of the available spectrograms. For merged (H1,L1)-spectrograms of the LIGO detectors, a PFA $p_1$ derives from causality in $t_s$ given GW170817-GRB17081A. A statistically independent confirmation is presented in individual H1 and L1 analyses, in a second PFA $p_2$ of consistency in their respective observations of $t_s$. A combined PFA derives from their product since mean and (respectively) difference in timing are statistically independent. Applied to GW170817-GRB170817A, PFAs of event timing in $t_s$ produce $p_1=8.3\times 10^{-4}$ and $p_2=4.9\times 10^{-5}$ of a post-merger output ${\cal E}_{GW}\simeq 3.5\%M_\odot c^2$ ($p_1p_2=4.1\times 10^{-8}$, equivalent $Z$-score 5.48). ${\cal E}_{GW}$ exceeds $E_J$ of the hyper-massive neutron star in the immediate aftermath of GW170817, yet it is consistent with $E_J$ rejuvenated in delayed gravitational collapse to a Kerr black hole. Similar emission may be expected from energetic core-collapse supernovae producing black holes. (Abbr.)
