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Magnetic field amplification in hypermassive neutron stars via the magnetorotational instability

MPG-Autoren
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Siegel,  Daniel
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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1401.5275.pdf
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chapter14.pdf
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Zitation

Siegel, D., & Ciolfi, R. (2015). Magnetic field amplification in hypermassive neutron stars via the magnetorotational instability. In P. Nicolini (Ed.), 1st Karl Schwarzschild Meeting on Gravitational Physics (Springer Proceedings in Physics, 170) (pp. 119-124). Heidelberg u.a.: Springer.


Zitierlink: https://hdl.handle.net/11858/00-001M-0000-0027-A5F5-B
Zusammenfassung
Mergers of binary neutron stars likely lead to the formation of a hypermassive neutron star (HMNS), which is metastable and eventually collapses to a black hole. This merger scenario is thought to explain the phenomenology of short gamma-ray bursts (SGRBs). The very high energies observed in SGRBs have been suggested to stem from neutrino-antineutrino annihilation and/or from very strong magnetic fields created during or after the merger by mechanisms like the magnetorotational instability (MRI). Here, we report on results that show for the first time the development of the MRI in HMNSs in three-dimensional, fully general-relativistic magnetohydrodynamic simulations. This instability amplifies magnetic fields exponentially and could be a vital ingredient in solving the SGRB puzzle.