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@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"
}


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