@Article{SousaCoelAraś:2020:GrWaFa,
               author = "Sousa, Manoel Felipe and Coelho, Jaziel Gourlart and Ara{\'u}jo, 
                         Jos{\'e} Carlos Neves de",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         {Universidade Tecnologica Federal do Paran{\'a} (UTFPR)} and 
                         {Instituto Nacional de Pesquisas Espaciais (INPE)}",
                title = "Gravitational waves from fast-spinning white dwarfs",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2020",
               volume = "492",
               number = "4",
                pages = "5949--5955",
                month = "Mar.",
             keywords = "gravitational waves, stars: magnetic field, white dwarfs.",
             abstract = "Two mechanisms of gravitational waves (GWs) emission in 
                         fast-spinning white dwarfs (WDs) are investigated: accretion of 
                         matter and magnetic deformation. In both cases, the GW emission is 
                         generated by an asymmetry around the rotation axis of the star. 
                         However, in the first case, the asymmetry is due to the amount of 
                         accreted matter on the magnetic poles, while in the second case it 
                         is due to the intense magnetic field. We have estimated the GW 
                         amplitude and luminosity for three binary systems that have a 
                         fast-spinning magnetized WD, namely, AF Aquarii, AR Scorpii, and 
                         RX J0648.0-4418. We find that, for the first mechanism, the 
                         systems AI( Aquarii and RX J0648.0-4418 can be observed by the 
                         space detectors 13130 and DEMO if they have an amount of accreted 
                         mass of fim > 10-5 Mo. For the second mechanism, the three systems 
                         studied require that the WD have a magnetic field above 10`' G to 
                         emit GWs that can be detected by BBO. We also verified that, in 
                         both mechanisms, the gravitational luminosity has an irrelevant 
                         contribution to the spin-down luminosity of these three systems. 
                         Therefore, other mechanisms of energy emission arc needed to 
                         explain the spin-down of these objects.",
                  doi = "10.1093/mnras/staa205",
                  url = "http://dx.doi.org/10.1093/mnras/staa205",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
           targetfile = "sousa_gravitational.pdf",
        urlaccessdate = "27 abr. 2024"
}