The GRB–SLSN connection: misaligned magnetars, weak jet emergence, and observational signatures
The GRB–SLSN connection: misaligned magnetars, weak jet emergence, and observational signatures
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GRB-SLSN 连接：未对准的磁星、弱喷流出现和观测特征
DOI：
10.1093/mnras/sty013
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发表时间：
2017
影响因子：
4.8
通讯作者：
["B. Margalit
中科院分区：
文献类型：
--
作者：
["B. Margalit
多个观测证据支持贫氢超光度超新星（SLSNe）和长持续时间伽马射线暴（GRB）之间的联系。这两个事件都需要强大的中央能源，通常归因于毫秒磁星或吸积黑洞。 GRB-SLSN 链接提出了几个理论问题：造成这些不同现象的引擎有何区别？一台发动机能否在同一赛事中同时为 GRB 和发光 SN 提供动力？我们提出了磁星热化和射流形成的新统一模型：自转轴 (${\bf \Omega}$) 和磁偶极子 (${\bf \mu}$) 轴之间的不对准通过条纹赤道风的重新连接热化了一部分自旋功率，从而为超新星提供了有保证的“热”发射源。剩余的未热化能量为相对论性射流提供能量。在这张图中，GRB-SLSN 二分法直接链接到 ${\bf \Omega \cdot \mu}$。我们扩展了早期的工作，表明即使是光度较弱的相对论性喷流 $\sim10^{46}$ erg s$^{-1}$ 也可以在爆炸后数小时逃离不断膨胀的超新星喷射物，这意味着逃逸的相对论性喷流可能伴随着许多超超超新星喷射。我们计算这些喷流的观测特征。我们表明，当射流冲出喷射物表面时，它们可能会产生持续数小时的瞬态紫外线茧发射。寿命较长的光学/紫外信号可能源自从射流和喷射物壁之间的界面驱动的温和相对论风。这为一些 SLSNe 光变曲线（例如 LSQ14bdq）中观察到的次级早期极大值提供了新的解释。这种情景还预测了来自轴上喷流的持续时间极长的伽玛射线暴群体，可能类似于“喷流潮汐破坏事件”的群体，与一小部分超超星系核暴一致。
Multiple observational lines of evidence support a connection between hydrogen-poor superluminous supernovae (SLSNe) and long duration gamma-ray bursts (GRBs). Both events require a powerful central energy source, usually attributed to a millisecond magnetar or an accreting black hole. The GRB-SLSN link raises several theoretical questions: What distinguishes the engines responsible for these different phenomena? Can a single engine power both a GRB and a luminous SN in the same event? We propose a new unifying model for magnetar thermalization and jet formation: misalignment between the rotation (${\bf \Omega}$) and magnetic dipole (${\bf \mu}$) axes thermalizes a fraction of the spindown power by reconnection in the striped equatorial wind, providing a guaranteed source of "thermal" emission to power the supernova. The remaining un-thermalized power energizes a relativistic jet. In this picture, the GRB-SLSN dichotomy is directly linked to ${\bf \Omega \cdot \mu}$. We extend earlier work to show that even weak relativistic jets of luminosity $\sim10^{46}$ erg s$^{-1}$ can escape the expanding SN ejecta hours after the explosion, implying that escaping relativistic jets may accompany many SLSNe. We calculate the observational signature of these jets. We show that they may produce transient UV cocoon emission lasting a few hours when the jet breaks out of the ejecta surface. A longer-lived optical/UV signal may originate from a mildly-relativistic wind driven from the interface between the jet and the ejecta walls. This provides a new explanation for the secondary early-time maximum observed in some SLSNe light curves, such as LSQ14bdq. This scenario also predicts a population of GRB from on-axis jets with extremely long durations, potentially similar to the population of "jetted tidal disruption events", in coincidence with a small subset of SLSNe.
影响因子：
64.8
作者：
J. Greiner;P. Mazzali;D. A. Kann;T. Krühler;E. Pian;S. Prentice;F. Olivares E.;A. Rossi;S. Klose;S. Taubenberger;F. Knust;P. Afonso;C. Ashall;J. Bolmer;C. Delvaux;R. Diehl;J. Elliott;R. Filgas;J. Fynbo;J. Graham;A. N. Guelbenzu;S. Kobayashi;G. Leloudas;S. Savaglio;P. Schady;S. Schmidl;T. Schweyer;V. Sudilovsky;M. Tanga;A. Updike;Hendrik van Eerten;K. Varela
通讯作者：
J. Greiner;P. Mazzali;D. A. Kann;T. Krühler;E. Pian;S. Prentice;F. Olivares E.;A. Rossi;S. Klose;S. Taubenberger;F. Knust;P. Afonso;C. Ashall;J. Bolmer;C. Delvaux;R. Diehl;J. Elliott;R. Filgas;J. Fynbo;J. Graham;A. N. Guelbenzu;S. Kobayashi;G. Leloudas;S. Savaglio;P. Schady;S. Schmidl;T. Schweyer;V. Sudilovsky;M. Tanga;A. Updike;Hendrik van Eerten;K. Varela
影响因子：
4.8
作者：
S. Komissarov
通讯作者：
S. Komissarov
影响因子：
6.5
作者：
D. A. Kann;P. Schady;F. Olivares;S. Klose;A. Rossi;D. Perley;T. Kruhler;J. Greiner;A. N. Guelbenzu
通讯作者：
D. A. Kann;P. Schady;F. Olivares;S. Klose;A. Rossi;D. Perley;T. Kruhler;J. Greiner;A. N. Guelbenzu