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arxiv: 1509.09205 · v2 · pith:GLNZESQTnew · submitted 2015-09-30 · 🌌 astro-ph.HE · astro-ph.CO· astro-ph.SR· gr-qc· nucl-th

Efficient magnetic-field amplification due to the Kelvin-Helmholtz instability in binary neutron star mergers

Kenta Kiuchi , Pablo Cerd\'a-Dur\'an , Koutarou Kyutoku , Yuichiro Sekiguchi , Masaru Shibata This is my paper
classification 🌌 astro-ph.HE astro-ph.COastro-ph.SRgr-qcnucl-th
keywords binarymagnetic-fieldneutronamplificationenergyexploregtrsiminstability
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We explore magnetic-field amplification due to the Kelvin-Helmholtz instability during binary neutron star mergers. By performing high-resolution general relativistic magnetohydrodynamics simulations with a resolution of $17.5$ m for $4$--$5$ ms after the onset of the merger on the Japanese supercomputer "K", we find that an initial magnetic field of moderate maximum strength $10^{13}$ G is amplified at least by a factor of $\approx 10^3$. We also explore the saturation of the magnetic-field energy and our result shows that it is likely to be $\gtrsim 4 \times 10^{50}$ erg, which is $\gtrsim 0.1\%$ of the bulk kinetic energy of the merging binary neutron stars.

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