TY - JOUR A1 - del Valle, Maria Victoria A1 - Pohl, Martin T1 - Nonthermal emission from Stellar Bow Shocks JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - Since the detection of nonthermal radio emission from the bow shock of the massive runaway star BD +43 degrees 3654, simple models have predicted high-energy emission, at X-rays and gamma-rays, from these Galactic sources. Observational searches for this emission so far give no conclusive evidence but a few candidates at gamma-rays. In this work we aim at developing a more sophisticated model for the nonthermal emission from massive runaway star bow shocks. The main goal is to establish whether these systems are efficient nonthermal emitters, even if they are not strong enough yet to be detected. For modeling the collision between the stellar wind and the interstellar medium we use 2D hydrodynamic simulations. We then adopt the flow profile of the wind and the ambient medium obtained with the simulation as the plasma state for solving the transport of energetic particles injected in the system, as well as the nonthermal emission they produce. For this purpose we solve a 3D (two spatial vertical bar energy) advection-diffusion equation in the test-particle approximation. We find that a massive runaway star with a powerful wind converts 0.16%-0.4% of the power injected in electrons into nonthermal emission, mostly produced by inverse Compton scattering of dust-emitted photons by relativistic electrons, and second by synchrotron radiation. This represents a fraction of similar to 10(-5) to 10(-4) of the wind kinetic power. Given the better sensibility of current instruments at radio wavelengths, these systems are more prone to be detected at radio through the synchrotron emission they produce rather than at gamma energies. KW - gamma-rays: stars KW - hydrodynamics KW - radiation mechanisms: nonthermal KW - stars: winds, outflows Y1 - 2018 U6 - https://doi.org/10.3847/1538-4357/aad333 SN - 0004-637X SN - 1538-4357 VL - 864 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Zhang, Haocheng A1 - Chen, Xuhui A1 - Böttcher, Markus A1 - Guo, Fan A1 - Li, Hui T1 - Polarization swings reveal magnetic energy dissipation in blazars JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - The polarization signatures of blazar emissions are known to be highly variable. In addition to small fluctuations of the polarization angle around a mean value, large (greater than or similar to 180 degrees) polarization angle swings are sometimes observed. We suggest that such phenomena can be interpreted as arising from light travel time effects within an underlying axisymmetric emission region. We present the first simultaneous fitting of the multi-wavelength spectrum, variability, and time-dependent polarization features of a correlated optical and gamma-ray flaring event of the prominent blazar 3C279, which was accompanied by a drastic change in its polarization signatures. This unprecedented combination of spectral, variability, and polarization information in a coherent physical model allows us to place stringent constraints on the particle acceleration and magnetic field topology in the relativistic jet of a blazar, strongly favoring a scenario in which magnetic energy dissipation is the primary driver of the flare event. KW - galaxies: active KW - galaxies: jets KW - gamma-rays: galaxies KW - radiation mechanisms: nonthermal KW - relativistic processes Y1 - 2015 U6 - https://doi.org/10.1088/0004-637X/804/1/58 SN - 0004-637X SN - 1538-4357 VL - 804 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER -