Prospects for the Observation of Continuous Gravitational Waves from Deformed Fast-spinning White Dwarfs
arxiv(2024)
Abstract
There has been a growing interest within the astrophysics community in highly
magnetized and fast-spinning white dwarfs (WDs), commonly referred to as HMWDs.
WDs with these characteristics are quite uncommon and possess magnetic fields
⩾ 10^6 G, along with short rotation periods ranging from seconds to
just a few minutes. Based on our previous work, we analyze the emission of
Gravitational Waves (GWs) in HMWDs through two mechanisms: matter accretion and
magnetic deformation, which arise due to the asymmetry surrounding the star's
rotational axis. Here, we perform a thorough self-consistent analysis,
accounting for rotation and employing a realistic equation of state to
investigate the stability of stars. Our investigation focuses on the emission
of gravitational radiation from six rapidly spinning WDs: five of them are
situated within binary systems, while one is an AXP, proposed as a magnetic
accreting WD. Furthermore, we apply the matter accretion mechanism alongside
the magnetic deformation mechanism to assess the influence of one process on
the other. Our discoveries indicate that these WDs could potentially act as GW
sources for BBO and DECIGO, depending on specific parameters, such as their
mass, the angle (α) between the magnetic and rotational axes, and the
accumulated mass (δ m) at their magnetic poles, which is influenced by
the effect of matter accretion. However, detecting this particular class of
stars using the LISA and TianQin space detectors seems unlikely due to the
challenging combination of parameters such as a large δ m, a large
α angle and a small WD mass value.
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