@Article{GontijoMira:2020:MaWaEx,
author = "Gontijo, Adam Smith and Miranda, Oswaldo Duarte",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto
Nacional de Pesquisas Espaciais (INPE)}",
title = "Magnetohydrodynamic waves excited by a coupling between
gravitational waves and a strongly magnetized plasma in binaries
of neutron stars",
journal = "Physical Review D",
year = "2020",
volume = "102",
number = "4",
pages = "e043004",
month = "Aug.",
abstract = "Coalescence of binary neutron stars (BNSs) is one of the sources
of gravitational waves (GWs) able to be detected by ground-based
interferometric detectors. The event GW170817 was the first
observed in the gravitational and electromagnetic spectra, showing
through this joint analysis a certain compatibility with the
models of short gamma-ray bursts (sGRBs) to explain the signature
of this system. Due to the intense magnetic fields of the neutron
stars, the plasma magnetosphere stays strongly magnetized and the
propagation of the GW through plasma can excite
magnetohydrodynamic (MHD) modes such as Affven and magnetosonic
waves. The MHD modes carry energy and momentum through the plasma,
suggesting a mechanism to accelerate the matter during the
coalescence of the binaries, explaining some characteristics of
the fireball model of the sGRBs. We present a semianalytical
formalism to determine the energy transferred by the GW-MHD
interaction during the inspiral phase of the stars. Using the
inferred physical parameters for GW170817 and considering that the
magnetic fields on the surfaces of the stars are 10(8) T, we show
that the energy in the plasma can reach maximum value similar to
10(35) J (similar to 10(32) J) for the Alfven mode (magnetosonic
mode) if the angle formed between the background magnetic field
and the GW propagation direction is theta =pi/4. Particularly, for
theta= pi/2 only the magnetosonic mode is in coherence with the
GWs. In this case, the excited energy in the plasma reaches
maximum value similar to 10(36) J. If the magnetic field on the
surface of the progenitors of the event GW170817 was similar to 2
x 10(9) T then energies comparable to those inferred for the GRB
170817A could be obtained. In particular, our semianalytical
formalism show consistence with the results obtained by other
authors through full general relativistic magnetohydro-dynamics
(GRMHD) simulations.",
doi = "10.1103/PhysRevD.102.043004",
url = "http://dx.doi.org/10.1103/PhysRevD.102.043004",
issn = "1550-2368 and 1550-7998",
language = "en",
targetfile = "gontijo_magnetohydrodynamic.pdf",
urlaccessdate = "28 mar. 2024"
}