论文标题
在伽马射线爆发中过渡到麦克洛蛋白球体的证据
Evidence for the transition of a Jacobi ellipsoid into a Maclaurin spheroid in gamma-ray bursts
论文作者
论文摘要
在二进制驱动的Hypernova（BDHN）方案中，长伽马射线爆发（GRB）起源于灾难性事件，发生在二进制系统中，该系统由碳氧（CO）星和由近距离Orbit中的碳氧气（CO）恒星和中子星（NS）伴侣组成。 CO星的崩溃在其中心产生了新生儿NS（$ν$ ns）和超新星（SN）爆炸。由于后备和NS伴侣，弹出物中的物质都被吸收到$ν$ ns上，从而导致后者崩溃成黑洞（BH）。上述系统的每种成分都会导致GRB中可观察到的发射发作。特别是，$ν$ ns有望在GRB早期排放中出现（以下几乎是现代或叠加到超级层次的及时发射（UPE）阶段，但具有不同的光谱签名。在$ν$ ns-rise之后，$ν$ ns通过将能量注入扩展的弹出器，从而为持久发射提供余辉的发射，从而导致同步辐射。我们在这里表明，$ν$ ns-rise和随后在两个系统中的余辉发射，GRB 180720b和GRB 190114c，由麦克洛蛋白球体的旋转能量释放，从分支点开始，从分叉点开始到雅各布椭圆形序列。这意味着$ν$ ns从$ν$ ns-rise之前的三轴雅各比构型演变为轴向对称的麦克劳林配置。由于GRB发射之前的重力发射大量发射，三轴$ν$ NS配置是短暂的（少于一秒），并且可以原则上检测到位于距离距离$ 100 $ 100 $ MPC的来源的原则上。这似乎是BDHN I为长GRB供电的重力波排放的特定过程。
In the binary-driven hypernova (BdHN) scenario, long gamma-ray bursts (GRBs) originate in a cataclysmic event that occurs in a binary system composed of a carbon-oxygen (CO) star and a neutron star (NS) companion in close orbit. The collapse of the CO star generates at its center a newborn NS ($ν$NS), and a supernova (SN) explosion. Matter from the ejecta is accreted both onto the $ν$NS because of fallback and onto the NS companion, leading to the collapse of the latter into a black hole (BH). Each of the ingredients of the above system leads to observable emission episodes in a GRB. In particular, the $ν$NS is expected to show up (hereafter $ν$NS-rise) in the early GRB emission, nearly contemporary or superimposed to the ultrarelativistic prompt emission (UPE) phase, but with a different spectral signature. Following the $ν$NS-rise, the $ν$NS powers the afterglow emission by injecting energy into the expanding ejecta leading to synchrotron radiation. We here show that the $ν$NS-rise and the subsequent afterglow emission in both systems, GRB 180720B and GRB 190114C, are powered by the release of rotational energy of a Maclaurin spheroid, starting from the bifurcation point to the Jacobi ellipsoid sequence. This implies that the $ν$NS evolves from a triaxial Jacobi configuration, prior to the $ν$NS-rise, into the axially symmetric Maclaurin configuration observed in the GRB. The triaxial $ν$NS configuration is short-lived (less than a second) due to a copious emission of gravitational waves, before the GRB emission, and it could be in principle detected for sources located at distances closer than $100$ Mpc. This appears to be a specific process of emission of gravitational waves in the BdHN I powering long GRBs.
