相位分辨超高能发射为致密天体引擎与致密物质结构划定能量边界
Phase-Resolved Ultra-High-Energy Emission Defines an Energetic Boundary for Compact-Object Engines and Dense-Matter Structure
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- Instituto Tecnológico de Aeronáutica（巴西航空工艺大学）
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中文总结 AI 辅助
该研究通过LS I +61 303的相位分辨超高能发射，结合EoS筛选与潮汐诊断，确定了致密天体引擎与环境边界，表明中子星结构差异仅在特定条件下可观测区分。
中文摘要 AI 辅助
我们证明，来自LS I +61 303的相位分辨超高能发射定义了一个关键的能量边界，该边界将致密天体引擎、星周相互作用深度与致密物质结构联系起来。将GeV-TeV-UHE谱跃迁与轨道加速-透明度筛分以及针对116个经认证的EoS（物态方程）的分支分辨恒星序列相结合，我们发现测得的25-100 TeV尾主要约束星周环境，而更严苛的纯强子>1 TeV解释则触及物理的转动惯量分布。在2.0 kpc和1.4 M_sun条件下，后者给出I45,crit = 1.5504；在Pdot_ref = 3 x 10^-15 s s^-1下，116个EoS中有82个满足相应的能量边界。另外应用的潮汐诊断Lambda_1.4 <= 580有43个EoS满足，其中9个同时满足两个条件。这些模型跨越多个微观类别，但占据狭窄的结构区域，表明存在结构重叠而非选择出唯一的EoS族。独立的GeV功率预算测试要求在2.0 kpc处Pdot_rot >= 5.65 x 10^-14 f_Omega s s^-1。对于f_Omega ~ 1，源远高于UHE交叉点，EoS区分度消失。因此，UHE观测确定了引擎-环境区域，在该区域中子星结构的差异可成为观测上可区分的，而非定义通用的致密物质选择器。
英文摘要
We show that phase-resolved ultra-high-energy emission from LS I \(+61^\circ303\) defines a critical energetic boundary linking the compact-object engine, circumstellar interaction depth, and dense-matter structure. Combining the GeV--TeV--UHE spectral transition with an orbital acceleration--transparency sieve and branch-resolved stellar sequences for 116 certified EoS, we find that the measured \(25\)--\(100\) TeV component remains energetically viable for all 116 canonical-mass EoS and therefore does not discriminate among them. EoS discrimination arises only in the deliberately more demanding pure-hadronic \(>1\) TeV stress-test construction: at 2.0 kpc and \(1.4\,M_\odot\), this boundary gives \(I_{45,\rm crit}=1.5504\), with 82 of 116 EoS satisfying the energetic condition at\(\dot P_{\rm ref}=3\times10^{-15}\,{\rm s\,s^{-1}}\). A separately applied tidal diagnostic, \(Λ_{1.4}\leq580\), is satisfied by 43 EoS, with nine satisfying both conditions. These models span several microscopic classes but occupy a narrow structural region, indicating structural overlap rather than selection of a unique EoS family. A separate GeV power-budget test requires \(\dot P_{\rm rot}\gtrsim 5.65\times10^{-14}f_Ω\,{\rm s\,s^{-1}}\) at 2.0 kpc. For \(f_Ω\sim1\), the source lies well above the UHE crossing and the EoS discrimination disappears. The UHE observation therefore identifies the engine--environment regime in which differences in neutron-star structure can become observationally discriminating, rather than defining a universal dense-matter selector.
