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dc.contributor.authorZhang, Haocheng
dc.contributor.authorBöttcher, Markus
dc.contributor.authorDeng, Wei
dc.contributor.authorLi, Hui
dc.date.accessioned2017-04-13T08:25:24Z
dc.date.available2017-04-13T08:25:24Z
dc.date.issued2016
dc.identifier.citationZhang, H. et al. 2016. Polarization signatures of relativistic magnetohydrodynamic shocks in the blazar emission region. I. Force-free helical magnetic fields. Astrophysical journal, 817(1): Article no 63. [https://doi.org/10.3847/0004-637X/817/1/63]en_US
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357 (Online)
dc.identifier.urihttp://hdl.handle.net/10394/21389
dc.identifier.urihttps://doi.org/10.3847/0004-637X/817/1/63
dc.identifier.urihttp://iopscience.iop.org/article/10.3847/0004-637X/817/1/63/pdf
dc.description.abstractThe optical radiation and polarization signatures in blazars are known to be highly variable during flaring activities. It is frequently argued that shocks are the main driver of the flaring events. However, the spectral variability modelings generally lack detailed considerations of the self-consistent magnetic field evolution modeling; thus, so far the associated optical polarization signatures are poorly understood. We present the first simultaneous modeling of the optical radiation and polarization signatures based on 3D magnetohydrodynamic simulations of relativistic shocks in the blazar emission environment, with the simplest physical assumptions. By comparing the results with observations, we find that shocks in a weakly magnetized environment will largely lead to significant changes in the optical polarization signatures, which are seldom seen in observations. Hence an emission region with relatively strong magnetization is preferred. In such an environment, slow shocks may produce minor flares with either erratic polarization fluctuations or considerable polarization variations, depending on the parameters; fast shocks can produce major flares with smooth polarization angle rotations. In addition, the magnetic fields in both cases are observed to actively revert to the original topology after the shocks. All these features are consistent with observations. Future observations of the radiation and polarization signatures will further constrain the flaring mechanism and the blazar emission environmenten_US
dc.language.isoenen_US
dc.publisherIOPen_US
dc.subjectGalaxies: activeen_US
dc.subjectGalaxies: jetsen_US
dc.subjectGamma rays: galaxiesen_US
dc.subjectPolarizationen_US
dc.subjectRadiation mechanisms: non-thermalen_US
dc.subjectRelativistic processesen_US
dc.titlePolarization signatures of relativistic magnetohydrodynamic shocks in the blazar emission region. I. Force-free helical magnetic fieldsen_US
dc.typeArticleen_US
dc.contributor.researchID24420530 - Böttcher, Markus


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