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Monte Carlo modeling of multi-PeV protons acceleration in gamma-ray binaries with strong stellar wind magnetic field.

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Title: Monte Carlo modeling of multi-PeV protons acceleration in gamma-ray binaries with strong stellar wind magnetic field.
Authors: Petrov, A.E.1 (AUTHOR) a.e.petrov@mail.ioffe.ru, Bykov, A.M.1 (AUTHOR) byk@astro.ioffe.ru
Source: Advances in Space Research. Apr2026, Vol. 77 Issue 8, p8391-8405. 15p.
Subjects: Stellar winds, Particle acceleration, Binary stars, Monte Carlo method, Gamma rays
Abstract: Recently discovered sources of very high energy gamma-rays (above 100 TeV) must support efficient mechanisms that can accelerate particles to PeV energies. Some of these sources are likely identified with compact binary star systems that harbor a relativistic companion. In such systems, the zone of collision of the relativistic outflow from a neutron star or a black hole with the powerful magnetized wind of the massive star provides conditions for efficient particle acceleration. We present a new Monte Carlo model of particle acceleration in binaries containing a rotation-powered pulsar, based on the results of accurate modeling of the collision winds zone structure. Our model takes into account the anisotropy of particle transport in the strong large-scale magnetic field of the winds. We discuss three phases of particle acceleration: (i) Fermi I type at a single shock of the wind's termination; (ii) Fermi I type in the zone of colliding winds and (iii) particle upscattering by fast relativistic inhomogeneities of (sub-)AU spatial scale moving with high Lorentz-factor Γ > 2 in the shocked pulsar wind. We demonstrate that these systems can efficiently produce multi-PeV protons for pulsar spin-down luminosity below 10 36 erg s - 1 , significantly exceeding the maximum energies associated with the total magnetospheric potential. A sub-Gauss stellar wind magnetic field in the collision zone ≲ 0.5 G and Γ ∼ 3 are necessary to reach energies ∼ 20 PeV that are required to trigger photomeson gamma-ray and neutrino production in such systems. [ABSTRACT FROM AUTHOR]
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Database: Engineering Source
Description
Abstract:Recently discovered sources of very high energy gamma-rays (above 100 TeV) must support efficient mechanisms that can accelerate particles to PeV energies. Some of these sources are likely identified with compact binary star systems that harbor a relativistic companion. In such systems, the zone of collision of the relativistic outflow from a neutron star or a black hole with the powerful magnetized wind of the massive star provides conditions for efficient particle acceleration. We present a new Monte Carlo model of particle acceleration in binaries containing a rotation-powered pulsar, based on the results of accurate modeling of the collision winds zone structure. Our model takes into account the anisotropy of particle transport in the strong large-scale magnetic field of the winds. We discuss three phases of particle acceleration: (i) Fermi I type at a single shock of the wind's termination; (ii) Fermi I type in the zone of colliding winds and (iii) particle upscattering by fast relativistic inhomogeneities of (sub-)AU spatial scale moving with high Lorentz-factor Γ > 2 in the shocked pulsar wind. We demonstrate that these systems can efficiently produce multi-PeV protons for pulsar spin-down luminosity below 10 36 erg s - 1 , significantly exceeding the maximum energies associated with the total magnetospheric potential. A sub-Gauss stellar wind magnetic field in the collision zone ≲ 0.5 G and Γ ∼ 3 are necessary to reach energies ∼ 20 PeV that are required to trigger photomeson gamma-ray and neutrino production in such systems. [ABSTRACT FROM AUTHOR]
ISSN:02731177
DOI:10.1016/j.asr.2026.01.103