Gravitational waves from fast-spinning white dwarfs

Autor(es)

Sousa, Manoel F. ^[1] ; Coelho, Jaziel G. ^{[1, 2]} ; de Araujo, Jose C. N. ^[1]

Afiliação do(s) autor(es)

^[1] Inst Nacl Pesquisas Espaciais, Div Astrofis, Ave Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP - Brazil

^[2] Univ Tecnol Fed Parana, Dept Fis, BR-85884000 Medianeira, PR - Brazil

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 492, n. 4, p. 5949-5955, MAR 2020.
• Citações Web of Science: 6

Resumo

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. (AU)

• Processo FAPESP: 13/26258-4 - Matéria superdensa no universo
• Beneficiário: Manuel Máximo Bastos Malheiro de Oliveira
• Modalidade de apoio: Auxílio à Pesquisa - Temático