Gravitational waves from fast-spinning white dwarfs

Sousa, Manoel F.; Coelho, Jaziel G.

doi:10.1093/mnras/staa205

Cited by 20 publications

(15 citation statements)

References 64 publications

(124 reference statements)

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“…These are WD pulsars, so they can emit both EM and GW radiations. Recently, Sousa et al (2020a) attempted to explain the emission of GWs including the mass accretion from the binary companion as well as the magnetic deformation. However, their study lacked proper source modelling because they considered the magnetic field inside the WD to be a dipole only.…”

Section: Detection Of Wd Pulsarsmentioning

confidence: 99%

Resolving dichotomy in compact objects through continuous gravitational waves observation

Kalita

Mondal

Tout

et al. 2021

Monthly Notices of the Royal Astronomical Society

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More than two dozen soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) have been detected so far. These are isolated compact objects. Many of them are either found to be associated with supernova remnants or their surface magnetic fields are directly measured, confirming that they are neutron stars (NSs). However, it has been argued that some SGRs and AXPs are highly magnetized white dwarfs (WDs). Meanwhile, the existence of super-Chandrasekhar WDs has remained to be a puzzle. However, not even a single such massive WD has been observed directly. Moreover, some WD pulsars are detected in electromagnetic surveys and some of their masses are still not confirmed. Here we calculate the signal-to-noise ratio for all these objects, considering different magnetic field configurations and thereby estimate the required time for their detection by various gravitational wave (GW) detectors. For SGRs and AXPs, we show that, if these are NSs, they can hardly be detected by any of the GW detectors, while if they are WDs, big bang Observer (BBO), DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) and Advanced Laser Interferometer Antenna (ALIA) would be able to detect them within a few days to a year of integration, depending on the magnetic field strength and its configuration. Similarly, if a super-Chandrasekhar WD has a dominant toroidal field, we show that even Laser Interferometer Space Antenna (LISA) and TianQin would be able to detect it within one year of integration. We also discuss how GWs can confirm the masses of the WD pulsars.

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Section: Detection Of Wd Pulsarsmentioning

confidence: 99%

Resolving dichotomy in compact objects through continuous gravitational waves observation

Kalita

Mondal

Tout

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…On the other hand, recent detection of GWs from the merger events opens a new window in astronomy. Since a strong magnetic field and high rotation can increase the mass of a WD, such a WD, possessing a specific configuration, can emit GW efficiently (Kalita & Mukhopadhyay 2019b, 2020Sousa et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Gravitational Wave in f(R) Gravity: Possible Signature of Sub- and Super-Chandrasekhar Limiting-mass White Dwarfs

Kalita

Mukhopadhyay

2021

ApJ

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After the prediction of many sub-and super-Chandrasekhar (at least a dozen for the latter) limiting-mass white dwarfs (WDs), hence apparently a peculiar class of WDs, from the observations of luminosity of Type Ia supernovae, researchers have proposed various models to explain these two classes of WD separately. We earlier showed that these two peculiar classes of WD, along with the regular WD, can be explained by a single form of the f (R) gravity, whose effect is significant only in the high-density regime, and it almost vanishes in the low-density regime. However, since there is no direct detection of such a WD, it is difficult to single out one specific theory from the zoo of modified theories of gravity. We discuss the possibility of direct detection of such a WD in gravitational wave (GW) astronomy. It is well known that in f (R) gravity more than two polarization modes are present. We estimate the amplitudes of all the relevant modes for the peculiar and the regular WD. We further discuss the possibility of their detections through future-based GW detectors, such as LISA, ALIA, DECIGO, BBO, or the Einstein Telescope, and thereby put constraints on or rule out various modified theories of gravity. This exploration links the theory with possible observations through GW in f (R) gravity.

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“…More recently, in Refs. 1,2,35, it has been suggested that rotating magnetized WDs can emit continuous GWs with amplitudes possibly detected by upcoming GW detectors such as LISA, DECIGO and BBO. Here we revisit our two works [Refs.…”

Section: Introductionmentioning

confidence: 99%

“…Here we revisit our two works [Refs. 1,2], where we investigate two mechanisms of gravitational radiation emission in fast-rotating magnetized WD: matter accretion and magnetic deformation. In both cases, the emission in GW is produced by the asymmetry around the star's rotation axis.…”

Section: Introductionmentioning

confidence: 99%

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Gravitational Wave Emission by Accretion of Matter and Magnetic Deformation in Fast Rotating White Dwarfs

Sousa,

de Araujo,

Coelho

2021

Preprint

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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 −5 M . For the second mechanism, the three systems studied require that the WD has a magnetic field above ∼ 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.

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Gravitational waves from fast-spinning white dwarfs

Cited by 20 publications

References 64 publications

Resolving dichotomy in compact objects through continuous gravitational waves observation

Resolving dichotomy in compact objects through continuous gravitational waves observation

Gravitational Wave in f(R) Gravity: Possible Signature of Sub- and Super-Chandrasekhar Limiting-mass White Dwarfs

Gravitational Wave Emission by Accretion of Matter and Magnetic Deformation in Fast Rotating White Dwarfs

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