@InCollection{SousaAraśCoel:2023:GrWaFa,
               author = "Sousa, Manoel Felipe and Ara{\'u}jo, Jos{\'e} Carlos Neves de 
                         and Coelho, Jaziel G.",
                title = "Gravitational waves from fast-spinning white dwarfs",
            booktitle = "The Sixteenth Marcel Grossmann Meeting. On Recent Developments in 
                         Theoretical and Experimental General Relativity, Astrophysics, and 
                         Relativistic Field Theories",
            publisher = "World Scientific Publishing",
                 year = "2023",
               editor = "Ruffini, R. and Vereshchagin, G.",
                pages = "4461--4474",
             keywords = "Gravitational Waves, White Dwarfs, Magnetic Field, Rapid 
                         Rotation.",
             abstract = "We discuss some aspects of Sousa et al. [1, 2] concerning two 
                         mechanisms of gravitational wave (GW) emission in fast-spinning 
                         white dwarfs (WDs): 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 in 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, AE 
                         Aquarii, AR Scorpii and RX J0648.0-4418. In addition, we applied 
                         the magnetic deformation mechanism for SGRs/AXPs described as WD 
                         pulsars. We found that, for the first mechanism, the systems AE 
                         Aquarii and RX J0648.0-4418 can be observed by the space detectors 
                         BBO and DECIGO if they have an amount of accreted mass of 
                         \δm \≥ 10\−5M\⊙. For the second 
                         mechanism, the three systems studied require that the WD has a 
                         magnetic field above \∼ 109 G to emit GWs that can be 
                         detected by BBO. Furthermore, we found that some SGRs/AXPs as WD 
                         pulsars can be detected by BBO and DECIGO, whereas SGRs/AXPs as 
                         highly magnetized neutron stars are far below the sensitivity 
                         curves of these detectors.",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Universidade 
                         Tecnol{\'o}gica Federal do Paran{\'a} (UTFPR)}",
                  doi = "10.1142/9789811269776_0377",
                  url = "http://dx.doi.org/10.1142/9789811269776_0377",
                 isbn = "9789811269776",
             language = "en",
           targetfile = "
                         
                         sousa-et-al-2023-gravitational-waves-from-fast-spinning-white-dwarfs.pdf",
        urlaccessdate = "10 maio 2024"
}