黑洞双星V4641 Sgr（银河系拍电子伏加速器）中延伸激波外流的粒子加速与非热宽带光谱
Particle acceleration and non-thermal broadband spectrum of extended shocked outflows in black hole binary V4641 Sgr - a galactic pevatron
AI总结：
该研究结合MHD模拟与动力学蒙特卡罗模型，解释黑洞双星V4641 Sgr的多波段非热辐射，揭示其可能是PeV宇宙射线的强大来源。
AI中文摘要：
恒星质量黑洞以超爱丁顿率吸积时会产生强外流和最高拍电子伏（PeV）能量的非热辐射。近期，在已知会发生超爱丁顿爆发的银河系微类星体V4641 Sgr的环境中发现了甚高能（VHE）辐射。我们结合磁流体动力学（MHD）模拟与非线性动力学蒙特卡罗模型，重现了V4641 Sgr周围数十秒差距范围内观测到的射电、X射线和伽马射线辐射。所报道的多波段非热辐射可解释为窄跨相对论性极区喷流与准球形吸积盘风相互作用产生的强激波系统加速PeV电子所致，激波位置对应伽马射线和X射线的亮斑，其空间轮廓可通过专项观测检验。该模型预测，喷流的相当一部分动能会转化为TeV-PeV质子，表明这类系统在加速器活动周期内可能是PeV范围宇宙射线的强大来源。在此模型中，MeerKAT在V4641 Sgr中发现的蝴蝶结形结构与准球形吸积盘风终止面的射电辐射相关。新发布的（来自SRG/eROSITA全天巡天）和存档的（INTEGRAL及Swift BAT）X射线数据与模型定量一致，同时重现了H.E.S.S.、HAWC和LHAASO的VHE测量结果。更深的X射线观测将检验该加速器的间歇性运行，这与SS433/W50等更持续的源形成对比。
英文摘要：
Stellar mass black holes accreting at a super-Eddington rate produce strong outflows and non-thermal radiation up to PeV energy. Recently, very high energy (VHE) emission was discovered from the environment of the galactic microquasar V4641 Sgr, which is known to experience super-Eddington outbursts. We present MHD simulations supplemented with a nonlinear kinetic Monte Carlo model that reproduces the observed radio, X-ray, and gamma-ray emission from the region over tens of parsecs surrounding V4641 Sgr. The reported multi-wavelength non-thermal emission can be explained as produced by PeV electrons accelerated by a system of strong shock waves created by the interaction between a narrow trans-relativistic polar jet and a quasi-spherical accretion-disk wind. The shock positions are associated with bright spots of the gamma-ray and X-ray radiation, whose spatial profiles can be tested with dedicated observations. The model predicts that a sizable fraction of the jet's kinetic energy is channeled into TeV-PeV protons, suggesting that such systems might be powerful sources of PeV-range cosmic rays during the accelerator activity cycle. In this model, the bow-tie shape structure discovered by MeerKAT in V4641 Sgr is associated with the radio emission from the termination surface of the quasi-spherical accretion-disk wind. The newly presented (from the SRG/eROSITA all-sky survey) and archival (INTEGRAL and Swift BAT) X-ray data are quantitatively consistent with the model, and simultaneously reproduce VHE measurements with H.E.S.S., HAWC, and LHAASO. Deeper X-ray observations will provide a test of the intermittent operation of the accelerator, in contrast with more persistent sources such as SS433/W50.
