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Accurate evolutions of inspiralling and magnetized neutron-stars: equal-mass binaries

MPG-Autoren
http://pubman.mpdl.mpg.de/cone/persons/resource/persons20657

Giacomazzo,  Bruno
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons20670

Rezzolla,  Luciano
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Volltexte (frei zugänglich)

1009.2468
(Preprint), 2MB

PRD83_044014.pdf
(beliebiger Volltext), 6MB

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Zitation

Giacomazzo, B., Rezzolla, L., & Baiotti, L. (2011). Accurate evolutions of inspiralling and magnetized neutron-stars: equal-mass binaries. Physical Review D, 83(4): 044014. doi:10.1103/PhysRevD.83.044014.


Zitierlink: http://hdl.handle.net/11858/00-001M-0000-000F-1065-D
Zusammenfassung
By performing new, long and numerically accurate general-relativistic simulations of magnetized, equal-mass neutron-star binaries, we investigate the role that realistic magnetic fields may have in the evolution of these systems. In particular, we study the evolution of the magnetic fields and show that they can influence the survival of the hypermassive-neutron star produced at the merger by accelerating its collapse to a black hole. We also provide evidence that even if purely poloidal initially, the magnetic fields produced in the tori surrounding the black hole have toroidal and poloidal components of equivalent strength. When estimating the possibility that magnetic fields could have an impact on the gravitational-wave signals emitted by these systems either during the inspiral or after the merger we conclude that for realistic magnetic-field strengths B<~1e12 G such effects could be detected, but only marginally, by detectors such as advanced LIGO or advanced Virgo. However, magnetically induced modifications could become detectable in the case of small-mass binaries and with the development of gravitational-wave detectors, such as the Einstein Telescope, with much higher sensitivities at frequencies larger than ~2 kHz.