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@ARTICLE{delValle:417535,
      author       = {del Valle, M. V. and Pohl, M.},
      title        = {{N}onthermal {E}mission from {S}tellar {B}ow {S}hocks},
      journal      = {The astrophysical journal / 1},
      volume       = {864},
      number       = {1},
      issn         = {1538-4357},
      address      = {Chicago, Ill. [u.a.]},
      publisher    = {IOP Publ.},
      reportid     = {PUBDB-2018-05692},
      pages        = {19},
      year         = {2018},
      note         = {© The American Astronomical Society.},
      abstract     = {Since the detection of nonthermal radio emission from the
                      bow shock of the massive runaway star BD +43°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 + 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
                      ~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.},
      cin          = {$Z_THAT$},
      ddc          = {520},
      cid          = {$I:(DE-H253)Z_THAT-20210408$},
      pnm          = {613 - Matter and Radiation from the Universe (POF3-613)},
      pid          = {G:(DE-HGF)POF3-613},
      experiment   = {EXP:(DE-MLZ)NOSPEC-20140101},
      typ          = {PUB:(DE-HGF)16},
      UT           = {WOS:000443007700008},
      doi          = {10.3847/1538-4357/aad333},
      url          = {https://bib-pubdb1.desy.de/record/417535},
}