The feasibility of magnetic reconnection powered blazar flares from synchrotron self-Compton emission-猫眼课题宝

同步加速器自康普顿发射磁重联驱动耀斑耀斑的可行性

DOI：

发表时间：

2018

期刊：

Monthly notices of the Royal Astronomical Society

影响因子：

4.8

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

P. Morris;W. Potter;G. Cotter

在活动星系核的耀变体子类中，在分钟时间尺度上观察到了数量级的变化。这种快速的高能量耀斑通常很难用传统的激波加速模型来解释，这是因为由光穿越时间推断出的发射区尺寸很小。最近的粒子模拟（PIC）表明，磁重联可能提供一个可行的解释。在本文中，我们提出了一个宏观的发射模型的物理动机的PIC模拟，粒子加速的能量来源于重联磁场。我们跟踪的径向增长和相对速度的重新连接等离子体团，建模粒子加速和辐射损失，发生通过同步加速器和同步自康普顿（SSC）的排放。我们假设重连层由合并的等离子体团组成，它们在合并时生长。我们使用我们的模型，成功地适应BL Lacertae的2016 TeV耀斑，证明重连能够在观测到的时间尺度上产生TeV耀斑。我们发现，耀斑的光变曲线依赖于合并的时间尺度和磁化的发射等离子体。然而，我们的模型产生的SED都是同步加速器主导的，可观察到的重联等离子体团的半径与射流半径相当。我们的结论是，虽然重联供电SSC耀斑可以产生耀斑的正确的时间尺度，排放的主要来源不能SSC和所需的等离子体团的大小可能是令人难以置信的大。

Order of magnitude variability has been observed in the blazar sub-class of Active Galactic Nuclei on minute timescales. Such fast high energy flares are often difficult to explain with conventional shock acceleration models due to the small size of the emitting region inferred by the light crossing time. Recent particle-in-cell (PIC) simulations have shown that magnetic reconnection may offer a viable explanation. In this paper, we present a macroscopic emission model physically motivated by PIC simulations, where the energy for particle acceleration originates from the reconnecting magnetic field. We track the radial growth and relative velocity of a reconnecting plasmoid, modelling particle acceleration and radiative losses, which occur via synchrotron and synchrotron self-Compton (SSC) emission. We assume the reconnection layer consists of merging plasmoids, which grow as they merge. We use our model to successfully fit to the 2016 TeV flare of BL Lacertae, demonstrating that reconnection is able to produce TeV flares on the observed timescales. We find that the flaring light curve depends on the merge timescale and the magnetisation of the emitting plasma. However, the SEDs produced by our model are all synchrotron-dominated, and observable reconnection plasmoids have radii comparable to the jet radius. We conclude that while reconnection powered SSC flares can produce flares on the correct timescale, the primary source of emission cannot be SSC and the size of plasmoids required may be implausibly large.

Electron and Proton Acceleration in Trans-relativistic Magnetic Reconnection: Dependence on Plasma Beta and Magnetization

DOI： 10.3847/1538-4357/aac820

发表时间： 2018-03

期刊：

The Astrophysical Journal

影响因子： --

作者：

D. Ball;L. Sironi;F. Özel

通讯作者：

D. Ball;L. Sironi;F. Özel

Multiwavelength Observations of the Blazar BL Lacertae: A New Fast TeV Gamma-Ray Flare

DOI： 10.3847/1538-4357/aab35c

发表时间： 2018-02

期刊：

The Astrophysical Journal

影响因子： --

作者：

A. Abeysekara;W. Benbow;R. Bird;T. Brantseg;R. Brose;M. Buchovecky;J. Buckley;V. Bugaev;M. Connolly;W. Cui;W. Cui;M. Daniel;A. Falcone;Q. Feng;Q. Feng;J. Finley;L. Fortson;A. Furniss;G. Gillanders;I. Gunawardhana;M. Hütten;D. Hanna;O. Hervet;J. Holder;G. Hughes;T. Humensky;C. Johnson;P. Kaaret;P. Kar;M. Kertzman;F. Krennrich;M. Lang;T. T. Lin-T.;S. McArthur;P. Moriarty;R. Mukherjee;S. O’Brien;R. Ong;A. Otte;N. Park;A. Petrashyk;M. Pohl;E. Pueschel;J. Quinn;K. Ragan;P. Reynolds;G. Richards;E. Roache;C. Rulten;I. Sadeh;M. Santander;M. Santander;G. Sembroski;K. Shahinyan;S. Wakely;A. Weinstein;R. Wells;P. Wilcox;D. Williams;B. Zitzer;S. Jorstad;S. Jorstad;A. Marscher;M. Lister;Y. Kovalev;Y. Kovalev;A. Pushkarev;T. Savolainen;T. Savolainen;I. Agudo;S. Molina;J. Gómez;V. Larionov;G. Borman;A. Mokrushina;M. Tornikoski;A. Lähteenmäki;A. Lähteenmäki;W. Chamani;S. Enestam;S. Kiehlmann;T. Hovatta;Paul S. Smith;P. Pontrelli

通讯作者：

The feasibility of magnetic reconnection powered blazar flares from synchrotron self-Compton emission

同步加速器自康普顿发射磁重联驱动耀斑耀斑的可行性

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