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3D relativistic MHD simulations of the gamma-ray binaries

Published online by Cambridge University Press:  18 September 2024

Maxim Barkov Open the ORCID record for Maxim Barkov [Opens in a new window] ,
Evgeniy Kalinin  and
Maxim Lyutikov
Maxim Barkov*
Affiliation:
Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia
Evgeniy Kalinin
Affiliation:
Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia Moscow Institute of Physics and Technology, Dolgoprudny, Russia
Maxim Lyutikov
Affiliation:
Department of Physics and Astronomy, Purdue University, West Lafayette, USA
*
Corresponding author: Maxim Barkov; Email: [email protected]
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Abstract

In gamma-ray binaries neutron star is orbiting a companion that produces a strong stellar wind. We demonstrate that observed properties of ‘stellar wind’–‘pulsar wind’ interaction depend both on the overall wind thrust ratio, as well as more subtle geometrical factors: the relative direction of the pulsar’s spin, the plane of the orbit, the direction of motion, and the instantaneous line of sight. Using fully 3D relativistic magnetohydrodynamical simulations we find that the resulting intrinsic morphologies can be significantly orbital phase-dependent: a given system may change from tailward-open to tailward-closed shapes. As a result, the region of unshocked pulsar wind can change by an order of magnitude over a quarter of the orbit. We calculate radiation maps and synthetic light curves for synchrotron (X-ray) and inverse-Compton emission (GeV-TeV), taking into account $\gamma $–$\gamma $ absorption. Our modelled light curves are in agreement with the phase-dependent observed light curves of LS5039.

Keywords

Magnetohydrodynamicsshock wavesbinaries: closepulsars: generalgamma-rays: stars
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 41 , 2024 , e048
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of Astronomical Society of Australia

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