Gravitational Radiation from Pulsating White Dwarfs

Abstract

Rotating white dwarfs undergoing quasi-radial oscillations can emit gravitational radiation in a frequency range from 0.1 - 0.3 Hz. Assuming that the energy source for the gravitational radiation comes from the oblateness of the white dwarf induced by the rotation, the strain amplitude is found to be \sim 10^{-27} for a white dwarf at \sim 50 pc. The galactic population of these sources is estimated to be \sim 10^7, and may produce a confusion limited foreground for proposed advanced detectors in the frequency band between space-based and ground-based interferometers. Nearby oscillating white dwarfs may provide a clear enough signal to investigate white dwarf interiors through gravitational wave asteroseismology.

arXiv commentAccepted for Astrophysical Journal Letters. Changed value of branching ratio resulting in an order of magnitude drop in gravitational wave amplitudes

References in corpus (4)

• Possibility of Direct Measurement of the Acceleration of the Universe Using 0.1 Hz Band Laser Interferometer Gravitational Wave Antenna in Space
• The True Incidence of Magnetism among Field White Dwarfs
• Gravitational Radiation from Strongly Magnetized White Dwarfs
• Studies of Magnetic and Suspected-Magnetic Southern White Dwarfs

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• The gravitational wave radiation of pulsating white dwarfs revisited: the case of BPM 37093 and PG 1159-035
• A search for gravitational waves associated with the August 2006 timing glitch of the Vela pulsar