Relativistic single-particle scattering cross sections for strong electromagnetic waves in strongly magnetized plasma are computed for arbitrary polarization and angle, showing strong suppression and sub-unity optical depth for quasi-parallel propagation.
Thermoplastic waves in magnetars
3 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
Magnetar activity is generated by shear motions of the neutron star surface, which relieve internal magnetic stresses. An analogy with earthquakes and faults is problematic, as the crust is permeated by strong magnetic fields, which greatly constrain crustal displacements. We describe a new deformation mechanism that is specific to strongly magnetized neutron stars. The magnetically stressed crust begins to move because of a thermoplastic instability, which launches a wave that shears the crust and burns its magnetic energy. The propagating wave front resembles the deflagration front in combustion physics. We describe the conditions for the instability, the front structure and velocity, and discuss implications for observed magnetar activity.
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astro-ph.HE 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
MD simulations identify a universal post-break plastic flow in neutron star crusts at shear strains of 0.05-0.11, independent of initial crystal structure.
Plane-parallel analysis finds MRI operates in solids only when magnetic tension exceeds shear modulus, requiring spin frequencies ≳300 Hz for crust amplification in neutron-star mergers.
citing papers explorer
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Scattering of Strong Radio Waves by Particles in Strongly Magnetized Plasmas and Implications for Fast Radio Bursts
Relativistic single-particle scattering cross sections for strong electromagnetic waves in strongly magnetized plasma are computed for arbitrary polarization and angle, showing strong suppression and sub-unity optical depth for quasi-parallel propagation.
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Plasticity of Neutron Star Crusts
MD simulations identify a universal post-break plastic flow in neutron star crusts at shear strains of 0.05-0.11, independent of initial crystal structure.
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Magneto-rotational instabilities in solids: application to neutron-star crusts
Plane-parallel analysis finds MRI operates in solids only when magnetic tension exceeds shear modulus, requiring spin frequencies ≳300 Hz for crust amplification in neutron-star mergers.