Timescales for Detecting Magnetized White Dwarfs in Gravitational Wave Astronomy

TL;DR

This paper explores the potential for detecting highly magnetized, rotating white dwarfs via gravitational waves with future detectors, analyzing emission timescales and detection prospects based on magnetic field properties.

Contribution

It provides a detailed analysis of the timescales and conditions under which magnetized white dwarfs emit detectable gravitational waves, highlighting future detection possibilities.

Findings

White dwarfs with strong magnetic fields can emit gravitational waves detectable by future observatories.

Detection depends on magnetic field geometry and strength, influencing emission timescales.

Future detectors like LISA and DECIGO can potentially observe these super-Chandrasekhar white dwarfs.

Abstract

Over the past couple of decades, researchers have predicted more than a dozen super-Chandrasekhar white dwarfs from the detections of over-luminous type Ia supernovae. It turns out that magnetic fields and rotation can explain such massive white dwarfs. If these rotating magnetized white dwarfs follow specific conditions, they can efficiently emit continuous gravitational waves and various futuristic detectors, viz. LISA, BBO, DECIGO, and ALIA can detect such gravitational waves with a significant signal-to-noise ratio. Moreover, we discuss various timescales over which these white dwarfs can emit dipole and quadrupole radiations and show that in the future, the gravitational wave detectors can directly detect the super-Chandrasekhar white dwarfs depending on the magnetic field geometry and its strength.