Volume 576, April 2015
|Number of page(s)||7|
|Published online||09 April 2015|
Cosmic rays in astrospheres
Institut für Theoretische Physik IV: Weltraum- und Astrophysik,
Ruhr-Universität Bochum, 44780
e-mail: email@example.com; firstname.lastname@example.org; email@example.com; firstname.lastname@example.org
2 Research Department, Plasmas with Complex Interactions, Ruhr-Universität Bochum, 44780 Bochum, Germany
3 Center for Space Research, North-West University, 2520 Potchefstroom, South Africa
e-mail: email@example.com; Stefan.Ferreira@nwu.ac.za; DuToit.Strauss@nwu.ac.za
4 Astronomisches Institut, Ruhr-Universität Bochum, 44780 Bochum, Germany
e-mail: firstname.lastname@example.org; email@example.com; firstname.lastname@example.org
Received: 1 October 2014
Accepted: 10 February 2015
Context. Cosmic rays passing through large astrospheres can be efficiently cooled inside these “cavities” in the interstellar medium. Moreover, the energy spectra of these energetic particles are already modulated in front of the astrospherical bow shocks.
Aims. We study the cosmic ray flux in and around λ Cephei as an example for an astrosphere. The large-scale plasma flow is modeled hydrodynamically with radiative cooling.
Methods. We study the cosmic ray flux in a stellar wind cavity using a transport model based on stochastic differential equations. The required parameters, most importantly, the elements of the diffusion tensor, are based on the heliospheric parameters. The magnetic field required for the diffusion coefficients is calculated kinematically. We discuss the transport in an astrospheric scenario with varying parameters for the transport coefficients.
Results. We show that large stellar wind cavities can act as sinks for the Galactic cosmic ray flux and thus can give rise to small-scale anisotropies in the direction to the observer.
Conclusions. Small-scale cosmic ray anisotropies can naturally be explained by the modulation of cosmic ray spectra in huge stellar wind cavities.
Key words: stars: winds, outflows / cosmic rays / hydrodynamics
© ESO, 2015
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