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Electron–positron pair plasma in TXS 0506+056 and the ‘neutrino flare’ in 2014–2015
Monthly Notices of the Royal Astronomical Society ( IF 4.7 ) Pub Date : 2020-08-06 , DOI: 10.1093/mnras/staa2284
N Fraija 1 , E Aguilar-Ruiz 1 , A Galván-Gámez 1
Affiliation  

The detection of a long flaring activity from blazar TXS 0506+056 in temporal and spatial coincidence with the energetic neutrino IceCube-170922A provided evidence about the photo-hadronic interactions in this source. However, analysis of the archival neutrino and multi-wavelength data from the direction of this blazar between September 2014 and March 2015 revealed a "neutrino flare" without observing quasi-simultaneous activity in the gamma-ray bands, posing challenges to established models. Electron-positron ($e^\pm$) pairs generated from the accretion disks have been amply proposed as a mechanism of bulk acceleration of sub-relativistic and relativistic jets. These pairs annihilate inside the source producing a line around the electron mass which is expected to be blueshifted in the observed frame (on Earth) and redshifted in the frame of the dissipation region of the jet. The redshifted photons in the dissipation region interact with accelerated protons, producing high-energy neutrinos that contribute significantly to the diffuse neutrino flux in the $\sim$ 10 - 20 TeV energy range in connection with gamma-rays from photo-pion process which can be detected by future MeV orbiting satellites. Based on this phenomenological model we can explain the "neutrino flare" reported in 2014 - 1015.

中文翻译:

TXS 0506+056 中的电子-正电子对等离子体和 2014-2015 年的“中微子耀斑”

在时间和空间上与高能中微子 IceCube-170922A 重合的耀变体 TXS 0506+056 的长时间燃烧活动的检测提供了有关该源中光强子相互作用的证据。然而,对 2014 年 9 月至 2015 年 3 月期间来自该耀变体方向的档案中微子和多波长数据的分析揭示了“中微子耀斑”,而没有观察到伽马射线带中的准同时活动,这对已建立的模型构成了挑战。吸积盘产生的正负电子 ($e^\pm$) 对已被充分提出作为亚相对论和相对论喷流的整体加速机制。这些对在源内湮灭,在电子质量周围产生一条线,预计在观察到的坐标系(地球上)中会发生蓝移,并在射流耗散区域的坐标系中发生红移。耗散区中的红移光子与加速质子相互作用,产生高能中微子,这些中微子对与来自光电-介子过程的伽马射线相关的在 $\sim$ 10 - 20 TeV 能量范围内的扩散中微子通量有显着贡献。被未来的 MeV 轨道卫星探测到。基于这个现象学模型,我们可以解释 2014 - 1015 年报道的“中微子耀斑”。产生高能中微子,这些中微子对 10 - 20 TeV 能量范围内的弥散中微子通量有显着贡献,这些中微子与来自光电粒子过程的伽马射线有关,可以被未来的 MeV 轨道卫星探测到。基于这个现象学模型,我们可以解释 2014 - 1015 年报道的“中微子耀斑”。产生高能中微子,这些中微子对 10 - 20 TeV 能量范围内的弥散中微子通量有显着贡献,这些中微子与来自光电粒子过程的伽马射线有关,可以被未来的 MeV 轨道卫星探测到。基于这个现象学模型,我们可以解释 2014 - 1015 年报道的“中微子耀斑”。
更新日期:2020-08-06
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