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Related Experiment Videos

Ultra-High-Energy Cosmic Rays from Young Neutron Star Winds.

Blasi, Epstein, Olinto

    The Astrophysical Journal
    |April 19, 2000
    PubMed
    Summary
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    Ultra-high-energy cosmic rays may originate from young, magnetized neutron stars, challenging extragalactic theories. These neutron stars can accelerate iron nuclei to extreme energies, explaining observed cosmic ray events.

    Area of Science:

    • Astrophysics
    • Particle Physics
    • Cosmic Ray Physics

    Background:

    • The origin of ultra-high-energy cosmic rays (UHECRs) remains a significant puzzle in astrophysics.
    • Observations show a lack of expected high-energy cutoff for cosmic rays above 10^20 eV, challenging extragalactic source models.
    • Photopion production off the cosmic microwave background typically limits cosmic ray energies.

    Purpose of the Study:

    • To propose an alternative, Galactic origin for UHECRs.
    • To investigate the potential of young, strongly magnetized neutron stars as accelerators for UHECRs.
    • To reconcile theoretical models with observational data of UHECRs.

    Main Methods:

    • Investigated the acceleration of iron nuclei by relativistic magnetohydrodynamic (MHD) winds from neutron stars.

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  • Modeled neutron star properties (spin period, magnetic field strength) required for extreme energy acceleration.
  • Simulated the propagation of accelerated iron nuclei through supernova remnants and Galactic magnetic fields.

    • Main Results:

    • Neutron stars with spin periods < 10 ms and magnetic fields of 10^12-10^14 G can accelerate iron nuclei beyond 10^20 eV.
    • Accelerated iron ions can traverse supernova remnants with minimal energy loss or spallation.
    • Simulated trajectories in Galactic magnetic fields are consistent with the observed isotropic arrival directions of UHECRs.

    Conclusions:

    • Young, strongly magnetized neutron stars are plausible sources of UHECRs.
    • This model challenges the prevailing extragalactic hypothesis for UHECR origins.
    • The proposed mechanism explains both the extreme energies and isotropic arrival distribution of observed UHECRs.