| Texto completo | |
| Autor(es): |
Sousa, M. F.
;
de Araujo, J. C. N.
;
Coelho, J. G.
Número total de Autores: 3
|
| Tipo de documento: | Artigo Científico |
| Fonte: | SIXTEENTH MARCEL GROSSMANN MEETING; v. N/A, p. 14-pg., 2023-01-01. |
| Resumo | |
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 delta m >= 10(-5) M-circle dot For the second mechanism, the three systems studied require that the WD has a magnetic field above similar to 10(9) 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. (AU) | |
| Processo FAPESP: | 15/15897-1 - Cherenkov Telescope Array - CTA |
| Beneficiário: | Luiz Vitor de Souza Filho |
| Modalidade de apoio: | Auxílio à Pesquisa - Temático |
| Processo FAPESP: | 13/26258-4 - Matéria superdensa no universo |
| Beneficiário: | Manuel Máximo Bastos Malheiro de Oliveira |
| Modalidade de apoio: | Auxílio à Pesquisa - Temático |